Modern optical engineering: the design of optical systems [3rd ed] 0071363602, 9780071363600

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Modern Optical Engineering

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Modern Optical Engineering The Design of Optical Systems

Warren J. Smith Chief Scientist, Kaiser Electro-Optics Inc. Carisbad, California and Consultant in Optics and Design

Third Edition

McGraw-Hill New York San Francisco Washington, D.C. Auckland Bogotá Caracas Lisbon London Madrid Mexico City Milan Montreal New Delhi San Juan Singapore Sydney Tokyo Toronto

Library of Congress Cataloging-in-Publication Data Smith, Warren J. Modern optical engineering / Warren J. Smith— 3rd ed. p. cm. Includes bibliographical references and index. ISBN 0-07-136360-2 1. Optical instruments—Design and construction. I. Title. TS513.S55 2000 621.36—dc21

00-032907

McGraw-Hill Copyright © 2000, 1990, 1966 by The McGraw-Hill Companies, Inc. Printed in the United States of America. Except as permitted under the United States Copyright Act of 1976, no part of this publication may be reproduced or distributed in any form or by any means, or stored in a data base or retrieval system, without the prior written permission of the publisher. 1 2 3 4 5 6 7 8 9 0 DOC/DOC 0 5 4 3 2 1 0 P/N 0-07-136379-3 PART OF ISBN 0-07-136360-2 The sponsoring editor of this book was Stephen S. Chapman. The editing supervisor was David E. Fogarty, and the production supervisor was Sherri Souffrance. It was set in New Century Schoolbook by Deirdre Sheean of McGraw-Hill’s Professional Book Group Hightstown composition unit. Printed and bound by R. R. Donnelley & Sons Company. This book was printed on recycled, acid-free paper containing a minimum of 50% recycled, de-inked fiber.

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Contents

Preface to the Third Edition xi Preface to the Second Edition xv

Chapter 1. General Principles 1.1 The Electromagnetic Spectrum 1.2 Light Wave Propagation 1.3 Snell’s Law of Refraction 1.4 The Action of Simple Lenses and Prisms on Wave Fronts 1.5 Interference and Diffraction 1.6 The Photoelectric Effect Bibliography Exercises

Chapter 2. Image Formation (First-Order Optics) 2.1 Introduction 2.2 Cardinal Points of an Optical System 2.3 Image Position and Size 2.4 Refraction of a Light Ray at a Single Surface 2.5 The Paraxial Region 2.6 Paraxial Raytracing through Several Surfaces 2.7 Calculation of the Focal Points and Principal Points 2.8 The “Thin Lens” 2.9 Mirrors 2.10 Systems of Separated Components 2.11 The Optical Invariant 2.12 Matrix Optics 2.13 The y-ybar Diagram 2.14 The Scheimpflug Condition 2.15 The Summary of Sign Conventions Bibliography Exercises

1 1 2 5 8 11 16 17 18

21 21 22 24 30 32 34 39 42 43 45 49 54 55 55 57 58 59

v

vi

Contents

Chapter 3. Aberrations 3.1 Introduction 3.2 The Aberration Polynomial and the Seidel Aberrations 3.3 Chromatic Aberrations 3.4 The Effect of Lens Shape and Stop Postion on the Aberrations 3.5 Aberration Variation with Aperture and Field 3.6 Optical Path Difference (Wave Front Aberrations) 3.7 Aberration Correction and Residuals 3.8 Ray Intercept Curves and the “Orders” of Aberrations Bibliography Exercises

Chapter 4. Prisms and Mirrors 4.1 Introduction 4.2 Dispersing Prisms 4.3 The “Thin” Prism 4.4 Minimum Deviation 4.5 The Achromatic Prism and the Direct Vision Prism 4.6 Total Internal Reflection 4.7 Reflection from a Plane Surface 4.8 Plane Parallel Plates 4.9 The Right-Angle Prism 4.10 The Roof Prism 4.11 Erecting Prism Systems 4.12 Inversion Prisms 4.13 The Penta Prism 4.14 Rhomboids and Beam Splitters 4.15 Plane Mirrors 4.16 The Design of Prism and Reflector Systems 4.17 Analysis of Fabrication Errors Bibliography

Chapter 5. The Eye

61 61 62 72 73 77 79 80 83 89 89

91 91 91 92 94 94 96 97 100 104 107 108 111 113 114 116 117 122 122

125

5.1 Introduction 5.2 The Structure of the Eye 5.3 Characteristics of the Eye 5.4 Defects of the Eye Bibliography Exercises

125 126 128 134 138 139

Chapter 6. Stops and Apertures

141

6.1 6.2 6.3 6.4 6.5

Introduction The Aperture Stop and Pupils The Field Stop Vignetting Glare Stops, Cold Stops, and Baffles

141 142 143 143 147

Contents 6.6 The Telecentric Stop 6.7 Apertures and Image Illumination—f -Number and Cosine-Fourth 6.8 Depth of Focus 6.9 Diffraction Effects of Apertures 6.10 Resolution of Optical Systems 6.11 Diffraction of a Gaussian (Laser) Beam 6.12 The Fourier Transform Lens and Spatial Filtering Bibliography Exercises

Chapter 7. Optical Materials and Interference Coatings 7.1 Reflection, Absorption, Dispersion 7.2 Optical Glass 7.3 Special Glasses 7.4 Crystalline Materials 7.5 Plastic Optical Materials 7.6 Absorption Filters 7.7 Diffusing Materials and Projection Screens 7.8 Polarizing Materials 7.9 Dielectric Reflection and Interference Filters 7.10 Reflectors 7.11 Reticles 7.12 Cements and Liquids Bibliography Exercises

Chapter 8. Radiometry and Photometry 8.1 Introduction 8.2 The Inverse Square Law; Intensity 8.3 Radiance and Lambert’s Law 8.4 Radiation into a Hemisphere 8.5 Irradiance Produced by a Diffuse Source 8.6 The Radiometry of Images; The Conservation of Radiance 8.7 Spectral Radiometry 8.8 Black Body Radiation 8.9 Photometry 8.10 Illumination Devices Bibliography Exercises

Chapter 9. Basic Optical Devices 9.1 9.2 9.3 9.4 9.5 9.6

Telescopes, Afocal Systems Field Lenses and Relay Stystems Exit Pupils, The Eye and Resolution The Simple Microscope or Magnifier The Compound Microscope Rangefinders

vii 150 151 154 157 160 163 168 168 169

173 173 178 183 187 188 192 195 198 200 209 211 213 214 216

219 219 220 221 222 223 225 230 231 237 243 248 249

251 251 255 257 267 269 271

viii

Contents 9.7 Radiometer and Detector Optics 9.8 Fiber Optics 9.9 Anamorphic Systems 9.10 Variable Power (Zoom) Systems 9.11 The Diffractive Surface Bibliography Exercises

Chapter 10. Optical Computation 10.1 Introduction 10.2 Paraxial Rays 10.3 Meridional Rays 10.4 General, or Skew, Rays: Spherical Surfaces 10.5 General, or Skew, Rays: Aspheric Surfaces 10.6 Coddington’s Equations 10.7 Aberration Determination 10.8 Third-Order Aberrations: Surface Contributions 10.9 Third-Order Aberrations: Thin Lenses; Stop Shift Equations Bibliography Exercises

Chapter 11. Image Evaluation 11.1 Introduction 11.2 Optical Path Difference: Focus Shift 11.3 Optical Path Difference: Spherical Aberration 11.4 Aberration Tolerances 11.5 Image Energy Distribution (Geometric) 11.6 Spread Functions—Point and Line 11.7 Geometric Spot Sizes Due to Spherical Aberration 11.8 The Modulation Transfer Function 11.9 Computation of the Modulation Transfer Function 11.10 Special Modulation Transfer Functions: Diffraction-Limited Systems 11.11 Radial Energy Distribution 11.12 Point Spread Functions for the Primary Aberrations Bibliography Exercises

Chapter 12. The Design of Optical Systems: General 12.1 Introduction 12.2 The Simple Meniscus Camera Lens 12.3 The Symmetrical Principle 12.4 Achromatic Telescope Objectives (Thin Lens Theory) 12.5 Achromatic Telescope Objectives (Design Forms) 12.6 The Diffractive Surface in Lens Design 12.7 The Cooke Triplet Anastigmat 12.8 A Generalized (Nonautomatic, Old-Fashioned) Design Technique

274 281 287 291 296 297 298

301 301 302 304 308 312 317 321 328 335 345 345

347 347 348 349 355 360 361 362 366 372 376 383 385 388 391

393 393 395 401 402 404 413 418 424

Contents 12.9 Automatic Design by Electronic Computer 12.10 Practical Considerations Bibliography Exercises

Chapter 13. The Design of Optical Systems: Particular 13.1 Telescope Systems and Eyepieces 13.2 Microscope Objectives 13.3 Photographic Objectives 13.4 Condenser Systems 13.5 Reflecting Systems 13.6 The Rapid Estimation of Blur Sizes for Simple Optical Systems Bibliography Exercises

Chapter 14. Some Forty Four More Lens Designs 14.1 Introduction 14.2 The Designs Bibliography

Chapter 15. Optics in Practice 15.1 Optical Manufacture 15.2 Optical Specifications and Tolerances 15.3 Optical Mounting Techniques 15.4 Optical Laboratory Practice Bibliography

Index

603

ix 431 435 436 438

439 439 447 453 470 474 491 499 502

503 503 504 504

549 549 559 575 580 599

Preface to the Third Edition

This is the third edition of Modern Optical Engineering. The first edition appeared in 1966; the second in 1990. Strictly by coincidence, this third edition will appear early in the third millennium. The changes from the second edition are rather modest, although quite numerous, evolutionary rather than revolutionary, as befits a book dealing with a science such as optics, which is well established and with a long history. As a historical note, when I enrolled in the Institute of Optics at the University of Rochester, I had an obligatory interview with the Dean, who carefully explained that optics was a very specialized and difficult course of study and that in the whole country there were less than a dozen potential employers for a graduate optical engineer. Despite the Dean’s gloom-and-doom prognostication, the future turned out amazingly well, and I have thoroughly enjoyed the practice of optical engineering and the people associated with it for over five and a half decades. Interestingly enough, in that period, the basics of optical engineering have changed very little, although the applications of optics have undergone rapid, extensive, dynamic, and fascinating changes. However, Snell’s law has not been repealed (although perhaps amended), and one who wishes to “practice optics” is still well advised to acquire a solid grounding in geometrical optics and optical engineering. Which brings us to the third edition. It is very flattering to an author to be asked by his publisher to prepare a new edition; it is especially so when the new edition is the third. But then the question that needs to be answered is, “What’s new and different?” The claim in the Preface of the Second Edition to some 1200 changes was met with, if not skepticism, then a slightly raised eyebrow on the part of one reviewer (a good friend and distinguished colleague). So you may be horrified to learn that I have again counted (and categorized) the changes. This time, depending on how you wish to classify them, the changes total 2104, plus or minus a few. xi

xii

Preface to the Third Edition

The basics of optical engineering are, as one might expect, little changed since 1990. I have yielded to common usage in replacing the symbol N for index of refraction with n (and I fondly hope that I have caught all the occurences of N). I also have changed the raytrace coordinates so that the optical axis is the z axis instead of the x axis. Believe it or not, these two items produced some 900 (admittedly minor) changes. While many of the other changes add new material, a large number are intended to clarify the existing text by the addition or modification of a word or two. Here are some of the more significant changes and additions: There is a new table of wavelength units and a new application of the invariant to afocal systems. The calculation of the entrance pupil location from the stop surface is detailed, and the Scheimpflug condition treatment is expanded to cover the cause and elimination of keystone distortion. Practical hints include blackening finishes as well as a list of no-nos (at least to the optics shop). The relationship between object-side and image-side numerical aperture (or fnumber) and the magnification is spelled out, as are the diffraction effects of gaussian beams and the often-overlooked differences between the focus and the waist of the beam. A section on the Fourier transform lens and spatial filtering has been added. A few practical hints on the procurement of plastic optics may save the reader a great deal of agony. Hot and cold mirrors are described. A new, simple, and easily understood derivation of the conservation of brightness and radiance has been added. New or expanded tables of brightness, illumination, and reflectance have been included, and the searchlight figure is improved. New equations for telescope (or afocal) component powers, eye relief, and eyepiece focus shift have been added, as well as a discussion of rod-lens endoscopes. A new deviation wedge device, a description of laser diode collimators, additional zoom-lens material, and a simplified discussion of certain diffractive surface effects have been added. Johnson’s law of recognition and resolution is described. The modulation transfer function as affected by coherent and partially coherent illumination systems is clearly explained. Specific equations for three-element apochromats are presented. The use of diffractive surfaces in lens design is illustrated by a design example of a hybrid refractive-diffractive achromatic singlet and an apochromatic doublet. Expressions for the efficiency and manufacturability of diffraction surfaces are given, including practical considerations with respect to shop/fabrication practices. Aberration effects in an eyepiece and eyepiece diopter adjustment equations are

Preface to the Third Edition

xiii

presented. Flat-field microscope objectives are described. An entirely new Chapter 14 has been added with 44 additional lens designs and prescriptions to supplement and expand on the lens design material in Chapters 12 and 13. Computer-controlled surfacing and magnetorheologic polishing are discussed. Single-point diamond turning of aspherics and the use of aspheric corrector plates are described. For those still wondering about the 2104 changes claimed earlier, here is a breakdown by type: 1. Change N to n and x to z.

900

Add, delete, or change: 2. A few words.

645

3. More than a few words.

120

4. Add a full sentence or an equation. 183 5. Add a new paragraph.

126

6. Add a new figure.

53

7. Add a new table.

4

8. Add a new chapter.

1

9. Add new references.

73

So there it is. The newer types of optics, such as diffractive, holographic, aspheric, gradient index, binary, etc., produce images and are used and incorporated into optical systems in much the same way as are the classical lenses and mirrors, although perhaps more powerfully and flexibly. Once one achieves a reasonable level of understanding (which need not be at an overwhelming level), these new devices can be incorporated readily into one’s optical system design. It is not unusual to find that the basics of the design of optical systems is actually little changed by these new, exciting, and tremendously useful developments. In conclusion, I hope that you, the reader, will enjoy the practice of optics as much as I have and that your practice proves as satisfying to you as mine has to me. I also hope that this third edition of Modern Optical Engineering is as useful to you as it has been to me. I wish you well. Warren J. Smith Vista, California

Preface to the Second Edition

This book is directed to the practicing engineer or scientist who requires effective practical technical information on optical systems and their design. The increase in the utilization of optical devices in such fields as alignment, metrology, automation, communication, and space and defense applications has brought about a need for technical people conversant with the optical field. Thus, many individuals whose basic training is in electronics, mechanics, physics, or mathematics find themselves in positions requiring a relatively advanced competence in optical engineering. It is the author’s hope that this volume will enable them to undertake their practice of optics soundly and with confidence. The book is based on the experiences of some fortyodd years in the actual practice of the design of optical systems, including commercial, experimental, and space and defense projects. I have tried to include and clearly explain the techniques which I found especially useful in my own work. Although the reader is presumed to be at least familiar with the optical material contained in a first-year physics course, the book begins with a general orientation chapter dealing with electromagnetic waves, Snell’s law, interference, diffraction, and the photoelectric effect. The second chapter goes quite deeply into image formation at the first-order (gaussian) level, and includes several numerical examples. The departures from first-order imagery represented by the aberrations are discussed in the third chapter. Prisms and mirrors are covered in both general and specific terms, in such a way that the reader can independently proceed beyond the standard systems. A chapter on the eye (as the basic “detector” involved in the vast majority of optical systems) follows. The chapter on stops and apertures covers the usual aperture, field, and glare stops and integrates the diffraction and resolution effects of xv

xvi

Preface to the Second Edition

apertures. The seventh chapter discusses optical materials and optical coatings, including the computation of the reflectance and transmittance of interference films. The chapter on radiation and photometry introduces the basic radiation concepts which are so necessary to a complete understanding of the relationship between the optics of a larger system and its performance. Chapter 9 discusses the basic tools of optics, the devices such as telescopes, microscopes, radiometers, variable-focus lenses, and the like, from which complete systems and instruments are designed. Chapters 10 through 13 are fairly advanced and contain sufficient material to permit the reader to undertake the complete design of an optical system. The chapter on optical computation covers ray-tracing through spherical and aspheric surfaces and includes techniques for determining the third-order aberrations. Image evaluation is discussed at length in Chapter 11, from both a geometrical and physical optics basis; the concept of the optical transfer function is introduced and computing techniques are demonstrated. Design procedures, both specific and generalized, are presented, and the individual design characteristics of a wide range of optical systems are discussed. Chapter 13 also includes a number of equations and charts which are of great value in preliminary engineering and proposal work and which permit a very rapid estimation of performance level for many basic optical systems. The final chapter of the book includes discussions of optical manufacturing processes, the specification, and tolerancing of optics for the shop, as well as brief discussions of optical-mechanics and laboratory practice. The general approach throughout has been to emphasize the application of basic optical principles to practice. Many numerical examples are included for the purpose of guiding the reader through typical engineering problems. Most chapters are followed by a set of exercises (and answers), designed to provide the reader with a close approximation to practical experience. The mathematical level required has been deliberately kept low; derivations are limited and are designed primarily to demonstrate either the technique of manipulation of optical quantities or the application of the relationships previously presented. The notation used is basically that of Conrady with modifications, since this is probably the most widely known and used system. This second edition of Modern Optical Engineering contains more than 1200 changes from the first edition. Some are major, some are quite subtle; some are additions, some are deletions. Many of the changes stem from the additional quarter-century of optical system design I have experienced since the original edition was undertaken. I am also indebted to the several thousand students to whom I have taught optics from this text; their questions and frequent puzzled

Preface to the Second Edition

xvii

expressions have inspired many of the corrections and rephrased expositions. Yet a third source has been the ongoing change in optical technology. Since it has proven quite difficult to amend Snell’s law, the changes in the optics of optical systems tend to be modest, also few and far between, but they do occur. It is with some regret that I have changed the sign convention for the ray slope. There were many advantages to the historical “optical” sign convention, but on balance they seemed to be outweighed by the confusion engendered in newcomers to the field by the contradiction between the “optical” convention and standard mathematical usage. The first edition of Modern Optical Engineering was written both as an instruction manual for newcomers to optical engineering and also as a reference work for those (myself included) already experienced in the field. Since the style, format, and organization of the first edition have been well received, the second edition follows them closely. A former student described it as “clear and easy to understand, brief and to the point, correct, and above all, useful.” It is my hope that this edition has retained, and added to, those qualities. I wish to acknowledge and express my gratitude to those who are truly responsible for the creation of this book: to my family, for their forbearance; to my teachers, for their knowledge and wisdom; to my colleagues, for their help, guidance, and shared experiences; to my students, for their enthusiasm and curiosity; and lastly, to many very special individuals too numerous to name, with the fond hope that you recognize yourselves here. PBGT. Warren J. Smith Vista, California

Chapter

1 General Principles

1.1 The Electromagnetic Spectrum This book deals with certain phenomena associated with a relatively narrow slice of the electromagnetic spectrum. Optics is often defined as being concerned with radiation visible to the human eye; however, in view of the recent expansion of optical applications in the regions of the spectrum on either side of the visible region, it seems not only prudent, but necessary, to include certain aspects of the infrared and ultraviolet regions in our discussions. The known electromagnetic spectrum is diagramed in Fig. 1.1 and ranges from cosmic rays to radio waves. All the electromagnetic radiations transport energy and all have a common velocity in vacuum of c  2.998  1010 cm/s. In other respects, however, the nature of the radiation varies widely, as might be expected from the tremendous range of wavelengths represented. At the short end of the spectrum we find gamma radiation with wavelengths extending below a billionth of a micron (one micron or micrometer  1 m  106 m) and at the long end, radio waves with wavelengths measurable in miles. At the short end of the spectrum, electromagnetic radiation tends to be quite particlelike in its behavior, whereas toward the long wavelength end the behavior is mostly wavelike. Since the optical portion of the spectrum occupies an intermediate position, it is not surprising that optical radiation exhibits both wave and particle behavior. The visible portion of this spectrum (Fig. 1.2) takes up less than one octave, ranging from violet light with a wavelength of 0.4 m to red light with a wavelength of 0.76 m. Beyond the red end of the spectrum lies the infrared region, which blends into the microwave region 1

2

Chapter One

Figure 1.1 The electromagnetic spectrum.

at a wavelength of about one millimeter. The ultraviolet region extends from the lower end of the visible spectrum to a wavelength of about 0.01 m at the beginning of the x-ray region. The wavelengths associated with the colors seen by the eye are indicated in Fig. 1.2. The ordinary units of wavelength measure in the optical region are the angstrom (Å); the millimicron (m), or nanometer (nm); and the micrometer (m), or micron (). One micron is a millionth of a meter, a millimicron is a thousandth of a micron, and an angstrom is one tenthousandth of a micron (see Table 1.1). Thus, 1.0 Å  0.1 nm  104 m. The frequency equals the velocity c divided by the wavelength, and the wavenumber is the reciprocal of the wavelength, with the usual dimension of cm1. 1.2 Light Wave Propagation If we consider light waves radiating from a point source in a vacuum as shown in Fig. 1.3, it is apparent that at a given instant each wave front is spherical in shape, with the curvature (reciprocal of the radius) decreasing as the wave front travels away from the point source. At a sufficient distance from the source the radius of the wave front may be regarded as infinite. Such a wave front is called a plane wave.

General Principles

3

Figure 1.2 The “optical” portion

of the electromagnetic spectrum.

TABLE 1.1

Commonly Used Wavelength Units

Centimeter

 102 meter

Millimeter

 103 meter

Micrometer

 106 meter

 103 millimeter

Micron

 106 meter

 103 millimeter

Millimicron

 1.0 nanometer  103 micron  106 millimeter  109 meter

Nanometer

 109 meter

Angstrom



1010

meter

 1.0 millimicron  0.1 nanometer

The distance between successive waves is of course the wavelength of the radiation. The velocity of propagation of light waves in vacuum is approximately 3  1010 cm/s. In other media the velocity is less than in vacuum. In ordinary glass, for example, the velocity is about twothirds of the velocity in free space. The ratio of the velocity in vacuum to the velocity in a medium is called the index of refraction of that medium, denoted by the letter n. velocity in vacuum Index of refraction n   velocity in medium

(1.1)

Both wavelength and velocity are reduced by a factor of the index; the frequency remains constant.

4

Chapter One

Ordinary air has an index of refraction of about 1.0003, and since almost all optical work (including measurement of the index of refraction) is carried out in a normal atmosphere, it is a highly convenient convention to express the index of a material relative to that of air (rather than vacuum), which is then assumed to have an index of exactly 1.0. The actual index of refraction for air at 15°C is given by 2,406,030 15,996 (n1) 108  8342.1     (1302) (38.92) where   1/ (  wavelength, in m). At other temperatures the index may be calculated from 1.0549 (n15°  1) (nt1)   (1  0.00366t) The change in index with pressure is 0.0003 per 15 lb/in2, or 0.00002/psi. If we trace the path of a hypothetical point on the surface of a wave front as it moves through space, we see that the point progresses as a straight line. The path of the point is thus what is called a ray of light. Such a light ray is an extremely convenient fiction, of great utility in understanding and analyzing the action of optical systems, and we shall devote the greater portion of this volume to the study of light rays. Note that the ray is normal to the wave front, and vice versa. The preceding discussion of wave fronts has assumed that the light waves were in a vacuum, and of course that the vacuum was isotropic, i.e., of uniform index in all directions. Several optical crystals are anisotropic; in such media wave fronts as sketched in Fig. 1.3 are not spherical. The waves travel at different velocities in different directions, and thus at a given instant a wave in one direction will be further from the source than will a wave traveling in a direction for which the media has a larger index of refraction.

Figure 1.3 Light waves radiat-

ing from a point source in an isotropic medium take a spherical form; the radius of curvature of the wave front is equal to the distance from the point source. The path of a point on the wave front is called a light ray, and in an isotropic medium is a straight line. Note also that the ray is normal to the wave front.

General Principles

5

Although most optical materials may be assumed to be isotropic, with a completely homogeneous index of refraction, there are some significant exceptions. The earth’s atmosphere at any given elevation is quite uniform in index, but when considered over a large range of altitudes, the index varies from about 1.0003 at sea level to 1.0 at extreme altitudes. Therefore, light rays passing through the atmosphere do not travel in exactly straight lines; they are refracted to curve toward the earth, i.e., toward the higher index. Gradient index optical glasses are deliberately fabricated to bend light rays in controlled curved paths. We shall assume homogeneous media unless specifically stated otherwise. 1.3

Snell’s Law of Refraction

Let us now consider a plane wave front incident upon a plane surface separating two media, as shown in Fig. 1.4. The light is progressing from the top of the figure downward and approaches the boundary surface at an angle. The parallel lines represent the positions of a wave front at regular intervals of time. The index of the upper medium we shall call n1 and that of the lower n2. From Eq. 1.1, we find that the velocity in the upper medium is given by v1  c/n1 (where c is the velocity in vacuum ≈ 3  1010 cm/s) and in the lower by v2  c/n2. Thus, the velocity in the upper medium is n2/n1 times the velocity in the lower, and the distance which the wave front travels in a given interval of time in the upper medium will also be n2/n1 times that in the lower. In Fig. 1.4 the index of the lower medium is assumed to be larger so that the velocity in the lower medium is less than that in the upper medium. At time t0 our wave front intersects the boundary at point A; at time t1  t0  t it intersects the boundary at B. During this time it has moved a distance c d1  v1 t   t (1.2a) n1 in the upper medium, and a distance

Figure 1.4 A plane wave front

passing through the boundary between two media of differing indices of refraction (n2  n1).

6

Chapter One

Figure 1.5

c d2  v2 t   t n2

(1.2b)

in the lower medium. In Fig. 1.5 we have added a ray to the wave diagram; this ray is the path of the point on the wave front which passes through point B on the surface and is normal to the wave front. If the lines represent the positions of the wave at equal intervals of time, AB and BC, the distances between intersections, must be equal. The angle between the wave front and the surface (I1 or I2) is equal to the angle between the ray (which is normal to the wave) and the normal to the surface XX′. Thus we have from Fig. 1.5 d1 d2 AB    BC   sin I1 sin I2 and if we substitute the values of d1 and d2 from Eq. 1.2, we get c t c t    n1 sin I1 n2 sin I2 which, after canceling and rearranging, yields n1 sin I1  n2 sin I2

(1.3)

This expression is the basic relationship by which the passage of light rays is traced through optical systems. It is called Snell’s law after one of its discoverers. Since Snell’s law relates the sines of the angles between a light ray and the normal to the surface, it is readily applicable to surfaces other

General Principles

7

than the plane which we used in the example above; the path of a light ray may be calculated through any surface for which we can determine the point of intersection of the ray and the normal to the surface at that point. The angle I1 between the incident ray and surface normal is customarily referred to as the angle of incidence; the angle I2 is called the angle of refraction. For all optical media the index of refraction varies with the wavelength of light. In general the index is higher for short wavelengths than for long wavelengths. In the preceding discussion it has been assumed that the light incident on the refracting surface was monochromatic, i.e., composed of only one wavelength of light. Figure 1.6 shows a ray of white light broken into its various component wavelengths by refraction at a surface. Notice that the blue light ray is bent, or refracted, through a greater angle than is the ray of red light. This is because n2 for blue light is larger than n2 for red. Since n2 sin I2  n1 sin I1  a constant in this case, it is apparent that if n2 is larger for blue light than red, then I2 must be smaller for blue than red. This variation in index with wavelength is called dispersion; when used as a differential it is written dn, otherwise dispersion is given by

n  n 1  n 2, where 1 and 2 are the wavelengths of the two colors of light for which the dispersion is given. Relative dispersion is given by n/(n  1) and, in effect, expresses the “spread” of the colors of light as a fraction of the amount that light of a median wavelength is bent.

Figure 1.6 Showing the dispersion of white light into its constituent colors by refraction (exaggerated for clarity).

8

Chapter One

Figure 1.7 Relationship between

a ray incident on a plane surface and the reflected and refracted rays which result.

All of the light incident upon a boundary surface is not transmitted through the surface; some portion is reflected back into the incident medium. A construction similar to that used in Fig. 1.5 can be used to demonstrate that the angle between the surface normal and the reflected ray (the angle of reflection) is equal to the angle of incidence, and that the reflected ray is on the opposite side of the normal from the incident ray (as is the refracted ray). Thus, for reflection, Snell’s law takes on the form Iincident  Ireflected

(1.4)

Figure 1.7 shows the relationship between a ray incident on a plane surface and the reflected and refracted rays which result. At this point it should be emphasized that the incident ray, the normal, the reflected ray, and the refracted ray all lie in a common plane, called the plane of incidence, which in Fig. 1.7 is the plane of the paper. 1.4 The Action of Simple Lenses and Prisms on Wave Fronts In Fig. 1.8 a point source P is emitting light; as before, the arcs centered about P represent the successive positions of a wave front at regular intervals of time. The wave front is incident on a biconvex lens consisting of two surfaces of rotation bounding a medium of (in this instance) higher index of refraction than the medium in which the

General Principles

9

source is located. In each interval of time the wave front may be assumed to travel a distance d1 in the medium of the source; it will travel a lesser distance d2 in the medium of the lens. (As in the preceding discussion, these distances are related by n1d1  n2d2.) At some instant, the vertex of the wave front will just contact the vertex of the lens surface at point A. In the succeeding interval, the portion of the wave front inside the lens will move a distance d2, while the portion of the same wave front still outside the lens will have moved d1. As the wave front passes through the lens, this effect is repeated in reverse at the second surface. It can be seen that the wave front has been retarded by the medium of the lens and that this retardation has been greater in the thicker central portion of the lens, causing the curvature of the wave front to be reversed. At the left of the lens the light from P was diverging, and to the right of the lens the light is now converging in the general direction of point P′. If a screen or sheet of paper were placed at P′, a concentration of light could be observed at this point. The lens is said to have formed an image of P at P′. A lens of this type is called a converging, or positive, lens. The object and image are said to be conjugates. Figure 1.8 diagrams the action of a convex lens—that is, a lens which is thicker at its center than at its edges. A convex lens with an index higher than that of the surrounding medium is a converging lens, in that it will increase the convergence (or reduce the divergence) of a wave front passing through it. In Fig. 1.9 the action of a concave lens is sketched. In this case the lens is thicker at the edge and thus retards the wave front more at the edge than at the center and increases the divergence. After passing through the lens, the wave front appears to have originated from the neighborhood of point P′, which is the image of point P formed by the lens. In this case, however, it would be futile to place a screen at P′ and

Figure 1.8 The passage of a wave front through a converging, or posi-

tive, lens element.

10

Chapter One

The passage of a wave front through a diverging, or negative, lens element.

Figure 1.9

expect to find a concentration of light; all that would be observed would be the general illumination produced by the light emanating from P. This type of image is called a virtual image to distinguish it from the type of image diagramed in Fig. 1.8, which is called a real image. Thus a virtual image may be observed directly or may serve as a source to be reimaged by a subsequent lens system, but it cannot be produced on a screen. The terms “real” and “virtual” also may be applied to rays, where “virtual” applies to the extended part of a real ray. The path of a ray of light through the lenses of Figs. 1.8 and 1.9 is the path traced by a point on the wave front. In Fig. 1.10 several ray paths have been drawn for the case of a converging lens. Note that the rays originate at point P and proceed in straight lines (since the media involved are isotropic) to the surface of the lens where they are refracted according to Snell’s law (Eq. 1.3.) After refraction at the second surface the rays converge at the image P′. (In practice the rays will converge exactly at P′ only if the lens surfaces are suitably chosen surfaces of rotation, usually nonspherical, whose axes are coincident and pass through P.) This would lead one to expect that the concentration of light at P′ would be a perfect point. However, the wave nature of light causes it to be diffracted in passing through the limiting aperture of the lens so that the image, even for a “perfect” lens, is spread out into a small disc of light surrounded by faint rings as discussed in Chap. 6. In Fig. 1.11 a wave front from a source so far distant that the curvature of the wave front is negligible is shown approaching a prism, which has two flat polished faces. As it passes through each face of the prism, the light is refracted downward so that the direction of propagation is deviated. The angle of deviation of the prism is the angle between the incident ray and the emergent ray. Note that the wave front remains plane as it passes through the prism. If the radiation incident on the prism consisted of more than one wavelength, the shorter-wavelength radiation would be slowed down more by the medium composing the prism and thus deviated through a greater angle. This is one of the methods used to separate different wavelengths of light and is, of course, the basis for Isaac Newton’s classic demonstration of the spectrum.

General Principles

11

Figure 1.10 Showing the relationship between light rays and the wave front

in passing through a positive lens element.

The passage of a plane wave front through a refracting prism.

Figure 1.11

1.5

Interference and Diffraction

If a stone is dropped into still water, a series of concentric ripples, or waves, is generated and spreads outward over the surface of the water. If two stones are dropped some distance apart, a careful observer will notice that where the waves from the two sources meet there are areas with waves twice as large as the original waves and also areas which are almost free of waves. This is because the waves can reinforce or cancel out the action of each other. Thus if the crests (or troughs) of two waves arrive simultaneously at the same point, the crest (or trough) generated is the sum of the two wave actions. However, if the crest of one wave arrives at the same instant as the trough of the other, the result is a cancellation. A more spectacular display of wave reinforcement can often be seen along a sea wall where an ocean wave which has struck the wall and been reflected back out to sea will combine with the next incoming wave to produce an eruption where they meet. Similar phenomena occur when light waves are made to interfere. In general, light from the same point on the source must be made to travel two separate paths and then be recombined, in order to produce optical interference. The familiar colors seen in soap bubbles or in oil films on wet pavements are produced by interference.

12

Chapter One

Figure 1.12

experiment.

Young’s diffraction

Young’s experiment, which is diagramed schematically in Fig. 1.12, illustrates both diffraction and interference. Light from a source to the left of the figure is caused to pass through a slit or pinhole s in an opaque screen. According to Huygens’ principle, the propagation of a wave front can be constructed by considering each point on the wave front as a source of new spherical wavelets; the envelope of these new wavelets indicates the new position of the wave front. Thus s may be considered as the center of a new spherical or cylindrical wave (depending on whether s is a pinhole or a slit), provided that the size of s is sufficiently small. These diffracted wave fronts from s travel to a second opaque screen which has two slits (or pinholes), A and B, from which new wave fronts originate. The wave fronts again spread out by diffraction and fall on an observing screen some distance away. Now, considering a specific point P on the screen, if the wave fronts arrive simultaneously (or in phase), they will reinforce each other and P will be illuminated. However, if the distances AP and BP are such that the waves arrive exactly out of phase, destructive interference will occur and P will be dark. If we assume that s, A, and B are so arranged that a wave front from s arrives simultaneously at A and B (that is, distance sA exactly equals distance sB), then new wavelets will start out simultaneously from A and B toward the screen. Now if distance AP exactly equals distance BP, or if AP differs from BP by exactly an integral number of wavelengths, the wave fronts will arrive at P in phase and will reinforce. If AP and BP differ by one-half wavelength, then the wave actions from the two sources will cancel each other. If the illuminating source is monochromatic, i.e., emits but a single wavelength of light, the result will be a series of alternating light and dark bands of gradually changing intensity on the screen (assuming that s, A, and B are slits), and by careful measurement of the geometry of the slits and the separation of the bands, the wavelength of the radiation may be computed. (The distance AB should be less than a millimeter and the distance from the slits to the screen should be to the order of a meter to conduct this experiment.)

General Principles

13

Figure 1.13 Geometry of Young’s

experiment.

With reference to Fig. 1.13, it can be seen that, to a first approximation, the path difference between AP and BP, which we shall represent by , is given by AB OP

  D Rearranging this expression, we get

D OP   AB

(1.5)

Now as Fig. 1.13 is drawn, it is obvious that the optical paths AO and BO are identical, so the waves will reinforce at O and produce a bright band. If we set in Eq. 1.5 equal to (plus or minus) one-half wavelength, we shall then get the value of OP for the first dark band ± D OP (1st dark)   2AB

(1.6)

and if we assume that the distance from slits to screen D is one meter, that the slit separation AB is one-tenth of a millimeter, and that the illumination is red light of a wavelength of 0.64 m, we get the following by substitution of these values in Eq. 1.6: ±104 0.64 103 ± 103 ±104     ±3.2 mm OP (1st dark)   1  2 10 2 2 Thus the first dark band occurs 3.2 mm above and below the axis. Similarly the location of the next light band can be found at 6.4 mm by setting equal to one wavelength, and so on. If blue light of wavelength 0.4 m were used in the experiment, we would find that the first dark band occurs at ±2 mm and the next bright band at ±4 mm. Now if the light source, instead of being monochromatic, is white and consists of all wavelengths, it can be seen that each wavelength will produce its own array of light and dark bands of its own particular spacing. Under these conditions the center of the screen will be illuminated by all wavelengths and will be white. As we proceed from the center, the first effect perceptible to the eye will be the dark band

14

Chapter One

for blue light which will occur at a point where the other wavelengths are still illuminating the screen. Similarly, the dark band for red light will occur where blue and other wavelengths are illuminating the screen. Thus a series of colored bands is produced, starting with white on axis and progressing through red, blue, green, orange, red, violet, green, and violet, as the path difference increases. Further from the axis, however, the various light and dark bands from all the visible wavelengths become so “scrambled” that the band structures blend together and disappear. Newton’s rings are produced by the interference of the light reflected from two surfaces which are close together. Figure 1.14 shows a beam of parallel light incident on a pair of partially reflecting surfaces. At some instant a wave front AA′ strikes the first surface at A. The point on the wave front at A travels through the space between the two surfaces and strikes the second surface at B where it is partially reflected; the reflected wave then travels upward to pass through the first surface again at C. Meanwhile the point on the wave front at A′ has been reflected at point C and the two paths recombine at this point. Now if the waves arrive at C in phase, they will reinforce; if they arrive one-half wavelength out of phase, they will cancel. In determining the phase relationship at C we must take into account the index of the material through which the light has traveled and also the phase change which occurs on reflection. This phase change occurs when light traveling through a low-index medium is reflected from the surface of a high-index medium; the phase is then abruptly changed by 180°, or one-half wavelength. No phase change occurs when the indices are encountered in reverse order. Thus with the relative indices as indicated in Fig. 1.14, there is a phase change at C for the light following the A′CD path, but no phase change at B for the light reflected from the lower surface.

Figure 1.14

General Principles

15

As in the case of Young’s experiment described above, the difference between the optical paths ABC and A′C determines the phase relationship. Since the index of refraction is inversely related to the velocity of light to a medium, it is apparent that the length of time a wave front takes to travel through a thickness d of a material of index n is given by t  nd/c (where c ≈ 3 1010 cm/s  velocity of light in vacuum). The constant frequency of electromagnetic radiation is given by c/ , so that the number of cycles which take place during the time t  nd/c is given by (c/ ) (nd/c) or nd/ . Thus, if the number of cycles are the same, or differ by an integral number of cycles, over the two paths of light traversed, the two beams of light will arrive at the same phase. In Fig. 1.14, the number of cycles for the path A′C is given by 1 2  n1 A′C/ (the one-half cycle is for the reflection phase change) and for the path ABC by n2 ABC/ ; if these numbers differ by an integer, the waves will reinforce; if they differ by an integer plus one-half, they will cancel. The use of cycles in this type of application is inconvenient, and it is customary to work in optical path length, which is the physical distance times the index and is a measure of the “travel time” for light. It is obvious that if we consider the difference between the two path lengths (arrived at by multiplying the above number of cycles by the wavelength ), exactly equivalent results are obtained when the difference is an integral number of wavelengths (for reinforcement) or an integral number plus one-half wavelength (for cancellation). Thus, for Fig. 1.14, the optical path difference (OPD) is given by OPD    n1 A′Cn2 ABC 2

(1.7)

or OPD    2n2t cos  2 when the phase change is taken into account by the /2 term. The term “Newton’s rings” usually refers to the ring pattern of interference bands formed when two spherical surfaces are placed in intimate contact. Figure 1.15 shows the convex surface of a lens resting on a plane surface. At the point of contact the difference in the optical paths reflected from the upper and lower surfaces is patently zero. The phase change on reflection from the lower surface causes the beams to rejoin exactly out of phase, resulting in complete cancellation and the appearance of the central “Newton’s black spot.” Some distance from the center the surfaces will be separated by exactly one-quarter wavelength, and this path difference of one-half

16

Chapter One

Figure 1.15

wavelength plus the phase change results in reinforcement, producing a bright ring. A little further from the center, the separation is one-half wavelength, resulting in a dark ring, and so on. Just as in Young’s experiment, the dark and bright bands for different wavelengths will occur at different distances from the center, resulting in colored circles near the point of contact which fade away toward the edge. A setup similar to Fig. 1.15 can obviously be used to measure the wavelength of light if the radius of curvature of the lens is known and a careful measurement of the diameters of the light and dark fringes is made. The spacing between the surfaces is the sagittal height (SH) of the radius, given by SH  R (R2  Y 2)1/2

(1.8)

where Y is the semidiameter of the ring measured. SH is equal to /4 for the first bright ring, /2 for the first dark ring, 3 /4 for the second bright ring, and so on. 1.6 The Photoelectric Effect In the preceding section, the discussion was based upon the assumption that light was wavelike in nature. This assumption provides reasonable explanations for reflection, refraction, interference, diffraction, and dispersion, as well as other effects. The photoelectric effect, however, seems to require for its explanation that light behave as if it consisted of particles. In brief, when short-wavelength light strikes a photoelectric material, it can knock electrons out of the material. As stated, this effect could be explained by the energy of the light waves exciting an electron sufficiently for it to break loose. However, when the nature of the

General Principles

17

incident radiation is modified, the characteristics of the emitted electrons change in an unexpected way. As the intensity of the light is increased, the number of electrons is increased just as might be expected. If the wavelength is increased, however, the maximum velocity of the electrons emitted is reduced; if the wavelength is increased beyond a certain value (this value is characteristic of the particular photoelectric material used), the maximum velocity drops to zero and no electrons are emitted, regardless of the intensity. The energy of a photon in electron volts is given by 1.24 divided by the wavelength in micrometers (microns). Thus the energy necessary to break loose an electron is not stored up until enough is available (as one would expect of the wavelike behavior of light.) The situation here is more analogous to a shower of particles, some of which have enough energy to break an electron loose from the forces which bind it in place. Thus the particles of shorter wavelength have sufficient energy to release an electron. If the intensity of light is increased, the number of electrons released is increased and their velocity remains unchanged. The longer-wavelength particles do not have enough energy to knock electrons loose, and when the intensity of the long-wavelength light is increased, the effect is to increase the number of particles striking the surface, but each particle is still insufficiently powerful to release an electron from its bonds. The apparent contradiction between the wave and particle behavior of light can be resolved by assuming that every “particle” has a wavelength associated with it which is inversely proportional to its momentum. This has proved true experimentally for electrons, protons, ions, atoms, and molecules; for example, an electron accelerated by an electric field of a few hundred volts has a wavelength of a few angstroms (104 m) associated with it. Reference to Fig. 1.1 indicates that this wavelength is characteristic of x-rays, and indeed, electrons of this wavelength are diffracted in the same patterns (by crystal lattices) as are x-rays. Bibliography Note: Titles preceded by an asterisk (*) are out of print. Born, M., and E. Wolf, Principles of Optics, Cambridge, England, Cambridge University Press, 1997. Brown, E., Modern Optics, New York, Reinhold, 1965. *Ditchburn, R., Light, New York, Wiley-Interscience, 1963. *Drude, P., Theory of Optics, New York, Dover, 1959. Greivenkamp, J. E., “Interference,” in Handbook of Optics, Vol. 1, New York, McGraw-Hill, 1995, Chap. 2.

18

Chapter One

*Hardy, A., and P. Perrin, The Principles of Optics, New York, McGrawHill, 1932. Hecht, E., and A. Zajac, Optics, Reading, Mass., Addison-Wesley, 1974. *Jacobs, D. Fundamentals of Optical Engineering, New York, McGrawHill, 1943. Jenkins, F., and H. White, Fundamentals of Optics, New York, McGraw-Hill, 1976. Kingslake, R., Optical System Design, New York, Academic, 1983. Levi, L., Applied Optics, New York, Wiley, 1968. Marathay, A. S., “Diffraction,” in Handbook of Optics, Vol. 1, New York, McGraw-Hill, 1995, Chap. 3. *Strong, J., Concepts of Classical Optics, New York, Freeman, 1958. Walker, B. H., Optical Engineering Fundamentals, New York, McGraw-Hill, 1995. *Wood, R., Physical Optics, New York, Macmillan, 1934. Exercises 1 What is the index of a medium in which light has a velocity of 2  1010 cm/sc? ANSWER:

1.5

2 What is the velocity of light in water, n  1.33? ANSWER:

2.26 1010 cm/s

3 A ray of light makes an angle of 30° with the normal to a surface. Find the angle to the normal after refraction if: (a) the ray is in air and the other material is glass, n  1.5. (b) the ray is in water and the other material is air. (c) the ray is in water and the other material is glass. ANSWER:

(a) 19.5°, (b) 41.7°, (c) 26.3°

4 Two 6-in-diameter optical flats are contacted at one edge and separated by a piece of paper (0.003-in thick) at the opposite edge. When illuminated by light of 0.000020-in wavelength, how many fringes will be seen? Assume normal incidence. ANSWER:

300 fringes

5 In Exercise 4, if the space between the flats is filled with water (n  1.333), how many fringes will be seen? ANSWER:

400 fringes

General Principles

19

6 The convex surface of a lens is in contact with a flat plate of glass. If the radius of the surface is 20 in, at what diameter will the first dark ring be seen? The second? The third? What are the ring diameters if the radius is 200 in? ANSWER:

0.040 in, 0.05657 in, 0.06928 in; 0.1265 in, 0.1789 in, 0.2191 in

Chapter

2 Image Formation (First-Order Options)

2.1

Introduction

The action of a lens on a wave front was briefly discussed in Sec. 1.4. Figures 1.8 and 1.9 showed how a lens can modify a wave front to form an image. A wave front is difficult to manipulate mathematically, and for most purposes the concept of a light ray (which is the path described by a point on a wave front) is much more convenient. In an isotropic medium, light rays are straight lines normal to the wave front, and the image of a point source is formed where the rays converge (or appear to converge) to a concentration or focus. In a perfect lens the rays converge to a point at the image. For purposes of calculation, an extended object may be regarded as an array of point sources. The location and size of the image formed by a given optical system can be determined by locating the respective images of the sources making up the object. This can be accomplished by calculating the paths of a number of rays from each object point through the optical system, applying Snell’s law (Eq. 1.3) at each raysurface intersection in turn. However, it is possible to locate optical images with considerably less effort by means of simple equations derived from the limiting case of the trigonometrically traced ray (as the angles involved approach zero). These expressions yield image positions and sizes which would be produced by a perfect optical system. The term “first-order” refers to a power series expansion equation which can be derived to define the intersection point of a ray in the

21

22

Chapter Two

image plane as a function of h, the position of the ray in the object plane, and y, the position of the ray in the aperture of the optical system. If the system is symmetrical about an axis (called the optical axis) the power series expansion has only odd power terms (in which the sum of the exponents of h and y add up to 1, 3, 5, etc.) The first-order terms of this expansion effectively describe the position and size of the image. (See Eqs. 3.1 and 3.2 for the equations.) First-order (or gaussian) optics is often referred to as the optics of perfect optical systems. The first-order equations can be derived by reducing the exact trigonometrical expressions for ray paths to the limit when the angles and ray heights involved approach zero. These equations are completely accurate for an infinitesimal threadlike region about the optical axis, known as the paraxial region. The value of first-order expressions lies in the fact that a well-corrected optical system will follow the first-order expressions almost exactly and also that the first-order image positions and sizes provide a convenient reference from which to measure departures from perfection. In addition, the paraxial expressions are linear and are much easier to use than the trigonometrical equations. We shall begin this chapter by considering the manner in which a “perfect” optical system forms an image, and we will discuss the expressions which allow the location and size of the image to be found when the basic characteristics of the optical system are known. Then we will take up the determination of these basic characteristics from the constructional parameters of an optical system. Finally, methods of image calculation by paraxial ray-tracing will be discussed. 2.2 Cardinal Points of an Optical System A well-corrected optical system can be treated as a “black box” whose characteristics are defined by its cardinal points, which are its first and second focal points, its first and second principal points, and its first and second nodal points. The focal points are those points at which light rays (from an infinitely distant axial object point) parallel to the optical axis* are brought to a common focus on the axis. If the rays entering the system and those emerging from the system are extended until they intersect, the points of intersection will define a surface, usually referred to as the principal plane. In a well-corrected optical system the principal surfaces are spheres, centered on the

*The optical axis is a line through the centers of curvature of the surfaces which make up the optical system. It is the common axis of rotation for an axially symmetrical optical system. Note that in real life, systems of more than two surfaces do not have a unique axis, because three or more real points are rarely aligned on a straight line.

Image Formation (First-Order Optics)

23

object and image. In the paraxial region where the distances from the axis are infinitesimal, the surfaces can be treated as if they were planes, hence the name, principal “planes.” The intersection of this surface with the axis is the principal point. The “second” focal point and the “second” principal point are those defined by rays approaching the system from the left. The “first” points are those defined by rays from the right. The effective focal length (efl) of a system is the distance from the principal point to the focal point. The back focal length (bfl), or back focus, is the distance from the vertex of the last surface of the system to the second focal point. The front focal length (ffl) is the distance from the front surface to the first focal point. These are illustrated in Fig. 2.1. The nodal points are two axial points such that a ray directed toward the first nodal point appears (after passing through the system) to emerge from the second nodal point parallel to its original direction. The nodal points of an optical system are illustrated in Fig. 2.2 for an ordinary thick lens element. When an optical system is bounded on both sides by air (as is true in the great majority of applications), the nodal points coincide with the principal points. Unless otherwise indicated, we will assume that our optical systems are axially symmetrical and are bounded by air. Equations 2.11 through 2.15 cover the case where the surrounding medium is not air.

Figure 2.1 Illustrating the location of the focal points and principal points of

a generalized optical system.

Figure 2.2 A ray directed toward

the first nodal point (N1) of an optical system emerges from the system without angular deviation and appears to come from the second nodal point (N2).

24

Chapter Two

The power of a lens or of an optical system is the reciprocal of its effective focal length; power is usually symbolized by the Greek letter phi (). If the focal length is given in meters, the power (in reciprocal meters) is measured in diopters. The dimension of power is reciprocal distance, e.g., in1, mm1, cm1, etc. 2.3 Image Position and Size When the cardinal points of an optical system are known, the location and size of the image formed by the optical system can be readily determined. In Fig. 2.3, the focal points F1 and F2 and the principal points P1 and P2 of an optical system are shown; the object which the system is to image is shown as the arrow AO. Ray OB, parallel to the system axis, will pass through the second focal point F2; the refraction will appear to have occurred at the second principal plane. The ray OF1C passing through the first focal point F1 will emerge from the system parallel to the axis. (Since the path of light rays is reversible, this is equivalent to starting a ray from the right at O′ parallel to the axis; the ray is then refracted through F1 in accordance with the definition of the first focal point in Sec. 2.2.) The intersection of these two rays at point O′ locates the image of point O. A similar construction for other points on the object would locate additional image points, which would lie along the indicated arrow O′A′. A plane object normal to the axis is imaged as a plane, also normal to the axis. See Sec. 2.14 for a tilted object. A third ray could be constructed from O to the first nodal point; this ray would appear to emerge from the second nodal point and would be parallel to the entering ray. If the object and image are both in air, the nodal points coincide with the principal points, and such a ray is drawn from O to P1 and from P2 to O′, as indicated by the dashed line in Fig. 2.3. At this point in our discussion, it is necessary to adopt a convention for the algebraic signs given to the various distances involved. The

Figure 2.3

Image Formation (First-Order Optics)

25

following conventions are used by most workers in the field of optics. There is nothing sacrosanct about these conventions, and many optical workers adopt their own, but the use of some consistent sign convention is a practical necessity. 1. Heights above the optical axis are positive (e.g., OA and P2 B). Heights below the axis are negative (P1C and A′O′). 2. Distances measured to the left of a reference point are negative; to the right, positive. Thus P1 A is negative and P2 A′ is positive. 3. The focal length of a converging lens is positive and the focal length of a diverging lens is negative.

Image position

Figure 2.4 is identical to Fig. 2.3 except that the distances have been given single letters; the heights of the object and image are labeled h and h′, the focal lengths are f and f ′, the object and image distances (from the principal planes) are s and s′, and the distances from focal point to object and image are x and x′, respectively. According to our sign convention, h f, f ′, x′, and s′ are positive as shown, and x, s, and h′ are negative. Note that the primed symbols refer to dimensions associated with the image and the unprimed symbols to those associated with the object. From similar triangles we can write (x) h    f (h′)

and

f′ h    (h′) x′

(2.1)

Setting the right-hand members of each equation equal and clearing fractions, we get ff ′   xx′

(2.2)

If we assume the optical system to be in air, then f will be equal to f ′ and

Figure 2.4

26

Chapter Two

f2 x′   x

(2.3)

This is the “newtonian” form of the image equation and is very useful for calculations where the locations of the focal points are known. If we substitute x  s  f and x′  s′  f in Eq. 2.3, we can derive another expression for the location of the image, the “gaussian” form. f 2   xx′   (s  f) (s′  f )   ss′  sf  s′f  f 2 Canceling out the f 2 terms and dividing through by ss′f, we get 1 1 1      s′ f s

(2.4)

or alternatively, sf s′   (s  f )

or

ss′ f  (s  s′)

(2.5)

Image size

The lateral (or transverse) magnification of an optical system is given by the ratio of image size to object size, h′/h. By rearranging Eq. 2.1, we get for the magnification m, x′ h′ f m      f h x

(2.6)

Substituting x  s  f in this expression to get h′ f m    h (s  f ) and noting from Eq. 2.5 that f/(sf ) is equal to s′/s, we find that s′ h′ m    h s

(2.7a)

s′  f (1  m)

(2.7b)

1 sf  1 m

(2.7c)

Other useful relations are

冢

冣

Image Formation (First-Order Optics)

27

Note that Eqs. 2.3 through 2.7 assume that both object and image are in air and also that Figs. 2.3 and 2.4 show a negative magnification. Longitudinal magnification is the magnification along the optical axis, i.e., the magnification of the longitudinal thickness of the object or the magnification of a longitudinal motion along the axis. If s1 and s2 denote the distances to the front and back edges of the object and s′1 and s′2 denote the distances to the corresponding edges of the image, then the longitudinal magnification 苶 m is, by definition, s′2  s′1 m 苶  s2  s1 Substituting Eq. 2.5 for the primed distances and manipulating, we get s′1 s′2 m (2.8) 苶     m1 m2 s1 s2 noting that m  s′/s. As (s′2  s′1) and (s2  s1) approach zero, then m1 approaches m2, and m  m2 苶

(2.9)

This indicates that longitudinal magnification is ordinarily positive and that object and image always move in the same direction. Example A

Given an optical system with a positive focal length of 10 in, find the position and size of the image formed of an object 5 in high which is located 40 in to the left of the first focal point of the system. Using the newtonian equation, we get, by substituting in Eq. 2.3,  f2 102 x′       2.5 in x 40 Therefore the image is located 2.5 in to the right of the second focal point. To find the image height, we use Eq. 2.6. h′ f 10 m        0.25 h x 40 h′  mh  (0.25) (5)  1.25 in Thus if the base of the object were on the optical axis and the top of the object 5 in above it, the base of the image would also lie on the axis and the image of the top would lie 1.25 in below the axis. The gaussian equations can be used for this calculation by noting that the distance from the first principal plane to the object is given by s  x  f  40  10  50; then, by Eq. 2.4,

28

Chapter Two

1 1 1 1 1           0.1  0.02  0.08 s′ f s 10 (50) 1 s′    12.5 in 0.08 and the image is found to lie 12.5 in to the right of the second principal plane (or 2.5 in to the right of the second focal point, in agreement with the previous solution). The height of the image can now be determined from Eq. 2.7a. h′ s′ 12.5 m         0.25 h s 50 h′  mh  (0.25) (5)  1.25 in Example B

If the object of Example A is located 2 in to the right of the first focal point, as shown in Fig. 2.5, where is the image and what is its height? Using Eq. 2.3, 102 f 2 x′      50 in x 2 Notice that the image is formed to the left of the second focal point; in fact, if the optical system is of moderate thickness, the image is to the left of the optical system and also to the left of the object. From Eq. 2.6 we get the magnification 10 h′ f m      5 h x 2 h′  mh  (5) (5)  25 in The magnification and image height are both positive. In this case the image is a virtual image. A screen placed at the image position will not have an image formed on it, but the image may be observed by viewing through the lens from the right. A positive sign for the lateral magnification of a simple lens indicates that the image formed is virtual; a neg-

Figure 2.5 Illustrating the for-

mation of a virtual image. See Example B.

Image Formation (First-Order Optics)

29

ative sign for the magnification of a simple lens indicates a real image. Figure 2.5 shows the relationships in this example. Example C

If the object of Example B is 0.1 in thick, what is the apparent thickness of the image? Since the lateral magnification was found to be 5 times in example B, the longitudinal magnification, by Eq. 2.9, is approximately 52, or 25. Thus the apparent image thickness is approximately 25 times (0.1 in), or 2.5 in. If an exact value for the apparent thickness is required, the image position for each surface of the object must be calculated. Assuming that the front of the object was given in Example B as 2 in to the right of the first focal point, then its rear surface must lie 1.9 in to the right of f1. Its image is located at f 2 100 x′      52.63 in 1.9 x to the left of the second focal point. Thus the distance between the image positions for the front and rear surfaces is 2.63 in, in reasonable agreement with the approximate result of 2.5 in. Had we computed the thickness for the case where the front and back surfaces of the object were 1.95 and 2.05 in from the focal point, the results from the exact and approximate calculations would have been in even better agreement, yielding an image thickness of 2.502 in. Optical systems not immersed in air

If the object and image are not in air, as assumed in the preceding paragraphs, the following equations should be used instead of the standard expressions of Eqs. 2.2 through 2.9. Assume an optical system with an object-side medium of index n, and an image-side medium of index n′. The first and second effective focal lengths, f and f′, respectively, may differ; they are related by f f′    n n′

(2.10)

The focal lengths can be determined by a ray-tracing calculation, just as with an air-immersed system. For example, f′  y1/u′k (see Eq. 2.34). Object and image distances

n′ n n n n′          f′ s f s s′

(2.11)

ff ′ x′   x

(2.12)

30

Chapter Two

Magnifications

x′ ns′ h′ f m        f′ n′s h x

(2.13)

for an object at infinity, h′  fup  f ′upn/n′

(2.14)

ff ′

s′ 2 m (note that m 苶    苶m) x2

s

(2.15)

Focal point to nodal point distance equals the other focal length. 2.4 Refraction of a Light Ray at a Single Surface As mentioned in Chap. 1, the path of a light ray through an optical system can be calculated from Snell’s law (Eq. 1.3) by the application of a modest amount of geometry and trigonometry. Figure 2.6 shows a light ray (GQP) incident on a spherical surface at point Q. The ray is directed toward point P where it would intersect the optical axis at a distance L from the surface if the ray were extended. At Q the ray is refracted by the surface and intersects the axis at P ′, a distance L′ from the surface. The surface has a radius R with center of curvature at C and separates two media of index n on the left and index n′ on the right. The light ray makes an angle U with the axis before refraction, U′ after refraction; angle I is the angle between the incident ray and the normal to the surface (HQC) at point Q, and angle I ′ is the angle between the refracted ray and the normal. Notice that plain or unprimed symbols are used for quantities before refraction at the surface; after refraction, the symbols are primed. The sign conventions which we shall observe are as follows: 1. A radius is positive if the center of curvature lies to the right of the surface. 2. As before, distances to the right of the surface are positive; to the left, negative. 3. The angles of incidence and refraction (I and I′) are positive if the ray is rotated clockwise to reach the normal. 4. The slope angles (U and U′) are positive if the ray is rotated clockwise to reach the axis. (Historical Note: Until the latter part of the twentieth century, the accepted convention for the sign of the slope was the reverse of the current one, and Fig. 2.6 was an “all-positive diagram.”)

Image Formation (First-Order Optics)

31

Figure 2.6 Refraction of a ray at a spherical surface.

5. The light travels from left to right. (In Fig. 2.6 all quantities are positive except U and U′, which are negative.) A set of equations which will allow us to trace the path for the ray may be derived as follows. From right triangle PAC, CA  (R  L) sin U

(2.16)

and from right triangle QAC, CA sin I   R

(2.17)

Applying Snell’s law (Eq. 1.3), we get the sine of the angle of refraction, n sin I′   sin I n′

(2.18)

The exterior angle QCO of triangle PQC is equal to U  I, and, as the exterior angle of triangle P′QC, it is also equal to U ′  I ′. Thus U  I  U′  I ′, and U′  UI  I′

(2.19)

From right triangle QA′C we get CA′ sin I′   R and substituting Eqs. 2.17 and 2.20 into Eq. 2.18 gives us

(2.20)

32

Chapter Two

n CA′   CA n′

(2.21)

Finally, the location of P′ is found by rearranging CA′  (R  L′) sin U′ from right triangle P′A′C into CA′ L′  R   sin U′

(2.22)

Thus, beginning with a ray defined by its slope angle U and its intersection with the axis L, we can determine the corresponding data, U′ and L′, for the ray after refraction by the surface. Obviously, this process could be applied surface by surface to trace the path of a ray through an optical system. 2.5 The Paraxial Region The paraxial region of an optical system is a thin threadlike region about the optical axis which is so small that all the angles made by the rays (i.e., the slope angles and the angles of incidence and refraction) may be set equal to their sines and tangents. At first glance this concept seems utterly useless, since the region is obviously infinitesimal and seemingly of value only as a limiting case. However, calculations of the performance of an optical system based on paraxial relationships are of tremendous utility. Their simplicity makes calculation and manipulation quick and easy. Since most optical systems of practical value form good images, it is apparent that most of the light rays originating at an object point must pass at least reasonably close to the paraxial image point. The paraxial relationships are the limiting relationships (as the angles approach zero) of the exact trigonometric relationships derived in the preceding section, and thus give locations for image points which serve as an excellent approximation for the imagery of a well-corrected optical system. Paradoxically, the paraxial equations are frequently used with relatively large angles and ray heights. This extension of the paraxial region is useful in estimating the necessary diameters of optical elements and in approximating the aberrations of the image formed by a lens system, as we shall demonstrate in later chapters. Although paraxial calculations are often used in rough preliminary work on optical systems and in approximate calculations (indeed, the term “paraxial approximation” is often used), the reader should bear in mind that the paraxial equations are perfectly exact for the paraxial region and that as an exact limiting case they are used in aberration determination as a basis of comparison to indicate how far a trigonometrically computed ray departs from its ideal location.

Image Formation (First-Order Optics)

33

The simplest way of deriving a set of equations for the paraxial region is to substitute the angle itself for its sine in the equations derived in the preceding section. Thus we get from Eq. 2.16

ca  (l  R)u

(2.23)

from Eq. 2.17

i  ca/R

(2.24)

from Eq. 2.18

i′  ni/n′

(2.25)

from Eq. 2.19

u′  u  i  i′

(2.26)

from Eq. 2.21

ca′  n ca/n′

(2.27)

from Eq. 2.22

l′  R  ca′/u′

(2.28)

Notice that the paraxial equations are distinguished from the trigonometric equations by the use of lowercase letters for the paraxial values. This is a widespread convention and will be observed throughout this text. Note also that the angles are in radian measure, not degrees. Equations 2.23 through 2.28 may be materially simplified. Indeed, since they apply exactly only to a region in which angles and heights are infinitesimal, we can totally eliminate i, u, and ca from the expressions without any loss of validity. Thus, if we substitute into Eq. 2.28, Eq. 2.27 for ca′ and Eq. 2.26 for u′, and continue the substitution with Eqs. 2.23, 2.24, and 2.25, the following simple expression for l′ is found: ln′R l′   (n′  n) l  nR

(2.29)

By rearranging we can get an expression which bears a marked similarity to Eq. 2.4 and Eq. 2.11 (relating the object and image distances for a complete lens system): (n′  n) n′ n      R l′ l

(2.30a)

These two equations are useful when the quantity of interest is the distance l′. If the object and image are at the axial intersection distances l and l′, the magnification is given by nl′ h′ (2.30b) m    n′l h In Sec. 2.2 we noted that the power of an optical system was the reciprocal of its effective focal length. In Eq. 2.30a the term (n′  n)/R is the power of the surface. A surface with positive power will bend

34

Chapter Two

(converge) a ray toward the axis; a negative-power surface will bend (diverge) a ray away from the axis. 2.6 Paraxial Raytracing through Several Surfaces The ynu raytrace

Another form of the paraxial equations is more convenient for use when calculations are to be continued through more than one surface. Figure 2.7 shows a paraxial ray incident on a surface at a height y from the axis, with the ray-axis intersection distances l and l′ before and after refraction. The height y in this case is a fictitious extension of the paraxial region, since, as noted, the paraxial region is an infinitesimal one about the axis. However, since all heights and angles cancel out of the paraxial expressions for the intercept distances (as indicated above), the use of finite heights and angles does not affect the accuracy of the expressions. For systems of modest aperture these fictitious heights and angles are a reasonable approximation to the corresponding values obtained by exact trigonometrical calculation. In the paraxial region, every surface approaches a flat plane surface, just as all angles approach their sines and tangents. Thus we can express the slope angles shown in Fig. 2.7 by u  y/l and u′  y/l′, or l  y/u and l′  y/u′. If we substitute these latter values for l and l′ into Eq. 2.30a, we get  (n′  n) nu n′u′      R y y and multiplying through by y, we find the slope after refraction. (n′  n) n′u′  nu  y  (2.31) R It is frequently convenient to express the curvature of a surface as the reciprocal of its radius, C  1/R; making this substitution, we have n′u′  nu  y (n′  n) C

Figure 2.7 Illustrating the rela-

tionship y  lu  l′u′ for paraxial rays.

(2.31a)

Image Formation (First-Order Optics)

35

To continue the calculation to the next surface of the system, we require a set of transfer equations. Figure 2.8 shows two surfaces of an optical system separated by an axial distance t. The ray is shown after refraction by surface #1; its slope is the angle u′1. The intersection heights of the ray at the surfaces are y1 and y2, respectively, and since this is a paraxial calculation, the difference between the two heights can be given by tu′1. Thus, it is apparent that n′1u′1 y2  y1  tu′1  y1  t  n′1

(2.32)

And if we note that the slope of the ray incident on surface #2 is the same as the slope after refraction by #1, we get the second transfer equation u2  u′1

or

n2 u2  n′1u′1

(2.33)

These equations can now be used to determine the position and size of the image formed by a complete optical system, as illustrated by the following example. Note that the paraxial ray heights and ray slopes are scalable (i.e., they may be multiplied by the same factor). The result of scaling is the data of another ray (which has the same axial intersection). Example D

Figure 2.9 shows a typical problem. The optical system consists of three surfaces, making a “doublet” lens whose radii, thicknesses, and indices are indicated in the figure. The object is located 300 mm to the left of the first surface and extends a height of 20 mm above the axis. The lens is immersed in air, so that object and image are in a medium of index n  1.0. The first step is to tabulate the parameters of the problem with the proper signs associated. Following the sign convention given above, we have the following:

2.8 Illustrating the transfer of a paraxial ray from surface to surface by y2  y1  tu′1. Note that although the surfaces are drawn as curved in the figure, mathematically they are treated as planes. Thus the ray is assumed to travel the axial spacing t in going from surface #1 to surface #2.

Figure

36

Chapter Two

Figure 2.9 Showing the rays traced in Example D.

h   20 mm l1  300 mm

n1  1.0

R1  50 mm

C1   0.02

t1  10 mm

n′1  n2  1.5

R2  50 mm

C2  0.02

t2  2 mm

n′2  n3  1.6

R3  plano

C3  0

n′3  1.0

The location of the image can be found by tracing a ray from the point where the object intersects the axis (O in the figure); the image will then be located where the ray recrosses the axis at O′. We can use any reasonable value for the starting data of this ray. Let us trace the path of the ray starting at O and striking the first surface at a height of 10 mm above the axis. Thus y1  10 and we get the initial slope angle by y1 10 u1      0.0333 l1 300 and since n1  1.0, n1u1  0.0333. The slope angle after refraction is obtained from Eq. 2.31a. n′1u′1  y1 (n′1  n1) C1  n1u1  10 (1.5  1.0) (0.02)  0.0333  0.1  0.0333 n′1u′1  0.0666 The ray height at surface #2 is found by Eq. 2.32. t1 (n′1u′1) y2  y1   n′1 10 (0.0666)  10   1.5

Image Formation (First-Order Optics)

37

 10  0.444 y2  9.555 Noting that n2u2  n′1u′1, the refraction at the second surface is carried through by n′2u′2  y2 (n′2  n2)C2  n2u2  9.555 (1.6  1.5) (0.02) 0.0666  0.019111  0.0666  0.047555 and the ray height at the third surface is calculated by 2(0.04755) t2 (n′2u′2) y3  y2    9.555   1.6 n′2  9.555  0.059444  9.496111 Since the last surface of the system is plane, i.e., of infinite radius, its curvature is zero and the product nu is unchanged at this surface: n′3u′3  y3 (n′3  n3) C3  n3u3  9.496111 (1.0  1.6) (0) 0.047555  0.047555 and n′3u′3 u′3    0.047555 n′3 Now the location of the image is given by the final intercept length l′, which is determined by 9.496111 y3 l′3     0.047555 u′3   199.6846 The execution of a long chain of calculations such as the preceding is much simplified if the calculation is arranged in a convenient table form. By ruling the paper in squares, a simple arrangement of the constructional parameters at the top of the sheet and the ray data below helps to speed the calculation and eliminate errors. The following table (Fig. 2.10) sets forth the curvatures, thicknesses, and indices of the lens in the first three rows; the next two rows contain the ray heights and index-slope angle products of the calculation worked out above.

38

Chapter Two

Figure 2.10

The image height can now be found by tracing a ray from the top of the object and determining the intersection of this ray with the image plane we have just computed. Such a ray is shown by the dashed line in Fig. 2.9. If we elect to trace the ray which strikes the vertex of the first surface, then y1 will be zero and the initial slope angle will be given by  (y1  h)  (0  20) u1      0.0666 l1 300 The calculation of this ray is indicated in the sixth and seventh rows of Fig. 2.10 and yields y3  0.52888…and n′3u′3  0.067555. The height of the image, h′ in Fig. 2.9, can be seen to equal the sum of the ray height at surface #3 plus the amount the ray climbs or drops in traveling to the image plane. 0.067555 n′3 u′3 h′  y3  l′3   0.52888  199.6846  1.0 n′3  14.0187 Notice that the expression used to compute h′ is analogous to Eq. 2.32; if we regard the image plane as surface #4 and the image distance l′3  199.6846 as the spacing between surfaces #3 and #4, Eq. 2.32 can be used to calculate y4, which is h′. Similarly, Eq. 2.32 can be used to determine the initial slope angle u1 by regarding the object plane as surface zero and rearranging the equation to solve for u′0  u1 as shown below: n′0 u′0 y1  y0  t0  n′0 h  y1 y1  y0 u′0  u1     l1 t0

Image Formation (First-Order Optics)

39

2.7 Calculation of the Focal Points and Principal Points In general, the focal lengths of an optical system can easily be calculated by tracing a ray parallel to the optical axis (i.e., with an initial slope angle u equal to zero) completely through the optical system. Then the effective focal length (efl) is minus the ray height at the first surface divided by the ray slope angle u′k after the ray emerges from the last surface. Similarly, the back focal length (bfl) is minus the ray height at the last surface divided by u′k. Using the customary convention that the data of the last surface of the system are identified by the subscript k, we can write y1 ef l   u′k

(2.34)

yk bf l   u′k

(2.35)

The cardinal points of a single lens element can be readily determined by use of the raytracing formulas given in the preceding section. The focal point is the point where the rays from an infinitely distant axial object cross the optical axis at a common focus. As indicated, this point can be located by tracing a ray with an initial slope (u1) of zero through the lens and determining the axial intercept. Figure 2.11 shows the path of such a ray through a lens element. The principal plane (p2) is located by the intersection of the extensions of the incident and emergent rays. The effective focal length (efl) or focal length (usually symbolized by f ), is the distance from p2 to f2 and, for the paraxial region, is given by y1 ef l  f   u′2 The back focal length (bfl) can be found from

Figure 2.11 A ray parallel to the axis is traced through an element to determine the effective focal length and back focal length.

40

Chapter Two

y2 bf l   u′2 Owing to the frequency with which these quantities are used, it is worthwhile to work up a single equation for each of them. If the lens has an index of refraction n and is surrounded by air of index 1.0, then n1  n′2  1.0 and n′1  n2  n. The surface radii are R1 and R2, and the surface curvatures are c1 and c2. The thickness is t. At the first surface, using Eq. 2.31a, n′1u′1  n1u1 (n′1  n1) y1c1  0  (n  1) y1c1 The height at the second surface is found from Eq. 2.32: t (n  1) y1c1 tn′1u′1 (n  1) y2  y1    y1    y1 1   tc1 n n n′1

冤

冥

And the final slope is found by Eq. 2.31a: n′2u′2  n′1u′1  y2(n′2  n2) c2 (n  1)   (n  1)y1c1  y1 1   tc1 (1  n) c2 n

冤

冥

(n  1) (1.0)u′2  u′2   y1(n  1) c1  c2  tc1c2  n

冤

冥

Thus the power  (or reciprocal focal length) of the element is expressed as (n  1) u′2 1       (n  1) c1  c2  tc1c2  n y1 f

冤

冥

(2.36)

or, if we substitute c  1/R, 1 t (n  1) 1 1     (n  1)      f R1R2 n R1 R2

冤

冥

(2.36a)

The back focal length can be found by dividing y2 by u′2 to get y2 ft (n  1) bf l    f   u′2 nr1

(2.37)

The distance from the second surface to the second principal point is just the difference between the back focal length and the effective focal length (see Fig. 2.11); this is obviously the last term of Eq. 2.37. The above procedure has located the second principal point and second focal point of the lens. The “first” points are found simply by substituting R1 for R2 and vice versa.

Image Formation (First-Order Optics)

41

The focal points and principal points for several shapes of elements are diagramed in Fig. 2.12. Notice that the principal points of an equiconvex or equiconcave element are approximately evenly spaced within the element. In the plano forms, one principal point is always at the curved surface, the other is about one-third of the way into the lens. In the meniscus forms shown, one of the principal points is completely outside the lens; in extreme meniscus shapes, both the principal points lie outside the lens and their order may be reversed from that shown. Note well that the focal points of the negative elements are in reversed order compared to a positive element. If the lens element is not immersed in air, we can derive a similar expression for it. Assuming that the object medium has an index of n1, the lens index is n2; and the image medium has an index of n3, then the two effective focal lengths and the back focal length can be calculated from (n2  n1) (n2  n3) (n2  n3) (n2  n1) t n1 n3          R1 R2 n2 R 1R2 f f′ f ′t (n2  n1) bf l  f′   n2 R1

Figure 2.12 The location of the focal points and principal points for several shapes of converging and diverging elements.

(2.38)

(2.39)

42

Chapter Two

Note that if n1 and n3 are equal to 1.0 (i.e., the index of air), these expressions reduce to Eqs. 2.36 and 2.37.

2.8 The “Thin Lens” If the thickness of a lens element is small enough so that its effect on the accuracy of the calculation may be neglected, the element is called a thin lens. The “thin lens” concept is an extremely useful one for the purposes of quick preliminary calculations and analysis and as a design tool. The focal length of a thin lens can be derived from Eq. 2.36 by setting the thickness equal to zero. 1   (n  1) (c1  c2) (2.40) f 1 1 1   (n  1)    f R1 R2

冢

冣

(2.40a)

Since the lens thickness is assumed to be zero, the principal points of a “thin lens” are coincident with the location of the lens. Thus, in computing object and image positions, the distances s and s′ of Eqs. 2.4, 2.5, 2.7, etc., are measured from the lens itself. The term (c1  c2) is often called the total curvature, or simply the curvature of the element. Example E

An object 10 mm high is to be imaged 50 mm high on a screen that is 120 mm distant. What are the radii of an equiconvex lens of index 1.5 which will produce an image of the proper size and location? The first step in the calculation is the determination of the focal length of the lens. Since the image is a real one, the magnification will have a negative sign, and by Eq. 2.7a we have h′ s′ 50 m    ()    h 10 s

or

s′  5s

For the object and image to be 120 mm apart, 120  s  s′  s  5s  6s s  20 mm and

s′  5s   100 mm

Substituting into Eq. 2.4 and solving for f, we get 1 1 1      100 f 20

Image Formation (First-Order Optics)

43

f  16.67 mm Noting that for an equiconvex lens R1  R2, we use Eq. 2.40a to solve for the radii 2 1 1 1    0.06  (n  1)     0.5  f R1 R2 R1 1 R1    16.67 mm 0.06

冢

冣

R2  R1  16.67 mm

2.9

Mirrors

A curved mirror surface has a focal length and is capable of forming images just as a lens does. The equations for paraxial raytracing (Eqs. 2.31 and 2.32) can be applied to reflecting surfaces by taking into account two additional sign conventions. The index of refraction of a material was defined in the first chapter as the ratio of the velocity of light in vacuum to that in the material. Since the direction of propagation of light is reversed upon reflection, it is logical that the sign of the velocity should be considered reversed, and the sign of the index reversed as well. Thus the conventions are as follows. 1. The signs of all indices following a reflection are reversed, so the index is negative when light travels right to left. 2. The signs of all spacings following a reflection are reversed if the following surface is to the left. Obviously if there are two reflecting surfaces in a system, the signs of the indices and spacings are changed twice and, after the second change, revert to the original positive signs, since the direction of propagation is again left to right. Figure 2.13 shows the locations of the focal and principal points of concave and convex mirrors. The ray from the infinitely distant source which defines the focal point can be traced as follows, setting n  1.0 and n′  1.0: nu  0

(since the ray is parallel to the axis)

(1  1) (n′  n) 2y n′u′  nu  y   0  y    R R R thus

44

Chapter Two

Figure 2.13 The location of the focal points for reflecting

surfaces.

2y n′u′ n′u′ u′       R 1 n′ The final intercept length is y R yR l′       u′ 2y 2 and we find that the focal point lies halfway between the mirror and its center of curvature. The concave mirror is the equivalent of a positive converging lens and forms a real image of distant objects. The convex mirror forms a virtual image and is equivalent to a negative element. Because of the index sign reversal on reflection, the sign of the focal length is reversed also and the focal length of a simple mirror is given by R f   2 so that the sign conforms to the convention of positive for converging elements and negative for diverging elements. Example F

Calculate the focal length of the Cassegrain mirror system shown in Fig. 2.14 if the radius of the primary mirror is 200 mm, the radius of the secondary mirror is 50 mm, and the mirrors are separated by 80 mm. Following our sign convention, the radii are both negative and the distance from primary to secondary mirror is also considered negative, since the light traverses this distance right to left. The index of the air is taken as 1.0 before the primary and after the secondary; between the two, the index is 1.0. Thus the optical data of the problem and the computation are set up and carried through as shown in Fig. 2.15. Careful attention to signs is necessary in this calculation to avoid mistakes.

Image Formation (First-Order Optics)

45

Cassegrain mirror system. The image formed by the primary mirror is the virtual object for the secondary mirror.

Figure 2.14

Figure 2.15

The focal length of the system is given by y1/u′2  1.0/0.002  500 mm. The final intercept distance (from R2 to the focus) is equal to y2/u′2  0.2/0.002  100 mm, and the focal point lies 20 mm to the right of the primary mirror. Notice that the (second) principal plane is completely outside the system, 400 mm to the left of the secondary mirror, and that this type of system provides a long focal length and a large image in a small, compact system. 2.10

Systems of Separated Components

It is often convenient to treat an optical system which is made up of separated elements or components (i.e., a group of elements treated as a unit) in terms of the component focal lengths and spacings instead of handling the system by means of surface-by-surface calculation. To this end we can introduce the paraxial ray height y into the equations of Sec. 2.3, just as we did in Sec. 2.6. An optical component (which may be made up of a number of elements) is shown in Fig. 2.16 with its object a distance s from the first principal plane and its image a distance s′ from the second principal plane. The principal planes are planes of unit magnification, in that the incident and emergent ray paths appear to strike (and emerge from) the same height on the first and second principal planes. Thus, in Fig. 2.16 a ray from the object point, which would (if extended) strike the first principal plane at a distance y from the axis, emerges from the last surface of the system as if it were coming from the same height y on the second principal plane. For this reason we can write the following relationships:

46

Chapter Two

Figure 2.16 The principal planes

are planes of unit magnification, so a ray appears to leave the second principal plane at the same height (y) that it appears to strike the first principal plane.

y u  s

and

y u′   s′

and substitute s  y/u and s′  y/u′ into Eq. 2.4: 1 1 1      s′ s f 1 u′ u      f y y y u′  u   f If we now replace the reciprocal focal length (1/f) with the component power , we get the first equation of the set: u′  u  y

(2.41)

The transfer equations to the next component in the system are the same as those used in the paraxial surface-by-surface raytrace of Sec. 2.6: y2  y1  du′1

(2.42)

u′1  u2

(2.43)

where y1 and y2 are the ray heights at the principal planes of components #1 and #2, u′1 is the slope angle after passing through component #1, and d is the axial distance from the second principal plane of component #1 to the first principal plane of component #2. Note that these equations are equally applicable to systems composed of either thick or “thin” lenses. Obviously, when applied to thin lenses, d becomes the spacing between elements, since the element and its principal planes are coincident. Focal lengths of two-component systems

The preceding equations may be used to derive compact expressions for the effective focal length and back focal length of a system comprised of two separated components. Let us assume that we have two lenses of powers a and b separated by a distance d (if the lenses

Image Formation (First-Order Optics)

47

are thin; if they are thick, d is the separation of their principal points). The system is sketched in Fig. 2.17. Beginning with a ray parallel to the axis which strikes lens a at ya, we have ua  0 u′a  0  yaa

by Eq. 2.41

yb  ya  dyaa  ya (1  da) u′b  yaa  ya (1  da) b

by Eq. 2.42 by Eq. 2.41

 ya (a  b  dab) The power (reciprocal focal length) of the system is given by ab 



u′b 1   a  b  dab ya fab

1 1 d       fa fb fa fb

(2.44)

and thus fa fb fab   (2.45) fa  fb  d The back focus distance (from the second principal point of b) is given by ya (1  da) y B  b   ya (a  b  dab) u′b (2.46) fb (fa  d) (1  d/fa)     fa  fb  d 1/fa  1/fb  d/fa fb By substituting fab/fa from Eq. 2.45, we get fab (fa  d) B   fa

(2.46a)

The front focus distance (ffd) for the system is found by reversing the raytrace (i.e., trace from right to left) or more simply by substituting fb for fa to get fab (fb  d) ()ffd   (2.46b) fb Frequently it is useful to be able to solve for the focal lengths of the components when the focal length, back focus distance, and spacing are given for the system. Manipulation of Eqs. 2.45 and 2.46a will yield

48

Chapter Two

Figure 2.17 Raytrace through two separated components to deter-

mine the focal length and back focus distance of the combination.

dfab fa   fab  B

(2.47)

dB fb   fab  B  d

(2.48)

General equations for two-component systems

Using the same technique, we can derive expressions which give us the solution to all two-component optical problems. There are two types of problems which occur. With reference to Fig. 2.18, the first type occurs when we are given the required system magnification, the positions of the two components, and the object-to-image distance (neglecting the spaces between the principal planes of the components.) Thus, knowing s, s′, d, and the magnification m, we wish to determine the powers (or focal lengths) of the two components, which are given by (ms  md  s′) A   msd

(2.49)

(d  ms  s′) B   ds′

(2.50)

In the second type of problem we are faced with the inverse case, in that we know the component powers, the desired object-to-image distance, and the magnification; we must determine the locations for the two components. Under these circumstances the mathematics result in a quadratic relationship, and thus there may be two solutions, one solution, or no solution (i.e., an imaginary solution.) The following

Image Formation (First-Order Optics)

49

Figure 2.18 A two-component system operating at finite conjugates.

quadratic equation in d (the spacing) is first solved for d [using the 2  4 standard equation x  ( b ± 兹b 苶ac) 苶/2a to solve O  ax2  bx  c]. (m  1)2 fA fB O  d2  dT  T (fA  fB)   m

(2.51)

Then s and s′ are easily determined from (m  1) d  T s   (m  1) mdA

(2.52)

s′  T  s  d

(2.53)

Thus Eqs. 2.44 through 2.53 constitute a set of expressions which can be used to solve any problem involving two components. Since twocomponent systems constitute the vast majority of optical systems, these are extremely useful equations. Note that a change of the sign of the magnification m from plus to minus will result in two completely different optical systems. They will produce the same enlargement (or reduction) of the image. One will have an erect, and the other an inverted, image, but one system may be significantly more suitable than the other for the intended application. 2.11 The Optical Invariant The optical invariant, or Lagrange invariant, is a constant for a given optical system, and it is a very useful one. Its numerical value may be calculated in any of several ways, and the invariant may then be used to arrive at the value of other quantities without the necessity of certain intermediate operations or raytrace calculations which would otherwise be required.

50

Chapter Two

Let us consider the application of Eq. 2.31a to the tracing of two rays through an optical system. One ray (the “axial” ray) is traced from the foot, or axial intercept, of the object; the other ray (the “oblique” ray) is traced from an off-axis point on the object. Figure 2.19 shows these two rays passing through a generalized system. At any surface in the system, we can write out Eq. 2.31a for each ray, using the subscript p to denote the data of the oblique ray. For the axial ray n′u′  nu  y (n′  n) c For the oblique ray n′u′p  nup  yp (n′  n) c We now extract the common term (n′  n)c from each equation and equate the two expressions: nup  n′u′p nu  n′u′ (n′  n) c     yp y Multiplying by yyp and rearranging, we get ypnu  ynup  ypn′u′  yn′u′p Note that on the left side of the equation the angles and indices are for the left side of the surface (that is, before refraction) and that on the right side of the equation the terms refer to the same quantities after refraction. Thus ypnu  ynup is a constant which is invariant across any surface. By a similar series of operations based on Eq. 2.32, we can show that (ypnu  ynup) for a given surface is equal to (ypnu  ynup) for the next surface. Thus this term is not only invariant across the surface but also across the space between the surfaces; it is therefore invariant throughout the entire optical system or any continuous part of the system. Invariant

Inv  ypnu  ynup  n (ypu  yup)

Figure 2.19

(2.54)

Image Formation (First-Order Optics)

51

The invariant and magnification

As an example of its application, we now write the invariant for the object plane and image plan of Fig. 2.19. In an object plane yp  h, n  n, y  0, and we get Inv  hnu  (0) nup  hnu In the corresponding image plane yp  h′, n  n′, y  0, and we get Inv  h′n′u′ (0) n′u′p  h′n′u′ Equating the two expressions gives hnu  h′n′u′

(2.55)

which can be rearranged to give a very generalized expression for the magnification of an optical system nu h′ m    n′u′ h

(2.56)

Equation 2.55 is, of course, valid only for the extended paraxial region; this relationship is sometimes applied to trigonometric calculations, where it takes the form hn sin u  h′n′ sin u′

(2.57)

Example G

We can apply the invariant to the calculation made in Example D by assuming that only the axial ray has been traced. The axial ray slope at the object was 0.0333…and the corresponding computed slope at the image was found to be 0.047555.…Since the object and image were both in air of index 1.0, we can find the image height from Eq. 2.56, h′ h′ nu 1.0 (0.0333…) m         1.0 (0.047555…) h 20 n′u′ 20 (0.0333) h′   0.047555) h′  14.0187 This value agrees with the height found in Example D by tracing a ray from the tip of the object to the tip of the image. The saving of time by the elimination of the calculation of this extra ray indicates the usefulness of the invariant.

52

Chapter Two

Image height for object at infinity

Another useful expression is derived when we consider the case of a lens with its object at infinity. At the first surface the invariant is Inv  ypn (0) y1nup  y1nup since the “axial” ray from an infinitely distant object has a slope angle u of zero. At the image plane yp is the image height h′, and y for the “axial” ray is zero; thus Inv  h′n′u′  (0) n′u′p  h′n′u′ Equating the two expressions for Inv, we get h′n′u′  y1nup ny1 h′  up  n′u′

(2.58)

which is useful for systems where the object and image are not in air. If both object and image are in air, we set n  n′  1.0, and recalling that f  y1/u′, we find (2.59)

h′  up f  tan up f

(for nonparaxial rays)

Telescopic magnification

If we evaluate the invariant at the entrance and exit pupils of a system, yp is (by definition) equal to zero, and the invariant becomes Inv  ynup  y′n′u′p where y is the pupil semidiameter, and up is the angular half field of view. For an afocal system we can equate the invariant at the entrance and exit pupils and then solve for the afocal (or telescopic) angular magnification to get u′p yn MP   up   y′n′ which indicates that the telescopic magnification is equal to the ratio of entrance pupil diameter to exit pupil diameter (assuming that n  n′). This is discussed further in Sec. 9.1. Data of a third ray from two traced rays

As one might expect from the preceding, a paraxial system is completely described by the ray data of any two unrelated rays. Thus,

Image Formation (First-Order Optics)

53

when we have traced two rays, we can determine the ray data of a third ray without further ray tracing, by using y苶  Ayp  By

(2.60)

u 苶  Aup  Bu

(2.61)

where y苶 and u 苶 refer to the third ray and yp, up, y, and u are the ray data for the oblique and axial rays as before. The constants A and B are determined by solving Eqs. 2.60 and 2.61 to get uyp y苶up  苶 n A     ( 苶yu  u (2.62) 苶y) uyp  yup Inv uyp  y苶up n 苶 B     (u 苶yp  y苶up) uyp  yup Inv

(2.63)

Equations 2.62 and 2.63 are evaluated for some surface in the optical system at which the height and slope data for all three rays are known (e.g., at the first surface or at the aperture stop). The constants A and B are inserted into Eqs. 2.60 and 2.61; the values of 苶y and u 苶 can then be determined for locations in the optical system at which the ray data for only the axial and oblique rays are known, by inserting this data in Eqs. 2.60 and 2.61. Focal length determination

As an example of the application of these equations, consider a system for which the axial and oblique rays have been traced for finite conjugates. The front, back, and effective focal lengths can be determined without additional raytracing as follows: We have values for the initial rays (y, u, yp, and up at the first surface) and for the final rays (y′, u′, y′p, and u′p, at the last surface); we wish to determine the final data (y 苶′ and u u  0. The applica苶′) for a third ray with starting data for 苶y  1 and 苶 tion of Eqs. 2.60 through 2.63 plus Eqs. 2.34 and 2.35 will yield  (yup  uyp) 苶y efl      uu′p  upu′ u 苶′

(2.64)

苶 y′  (upy′  uy′p) bf l     (2.65) uu′  u u′ u ′ p p 苶 Reversing the process by setting u 苶′  0 and y苶′  1, we get the (normally negative) value for the front focal length py  u′yp) y 苶  (u′  ffl   uup′  up u′ u 苶

(2.66)

54

Chapter Two

Most optical computer programs make use of Eqs. 2.60 to 2.63 to locate the entrance pupil when the aperture stop position is given and use Eqs. 2.64 to 2.66 to calculate the focal lengths. Such programs usually put a nominally infinitely distant object at a large, but finite, distance and thus cannot directly calculate the focal lengths without a special calculation. Aperture stop and entrance pupil

Another optical software application of this principle involves the determination of the entrance pupil location when the required location of the aperture stop is given. Again, assuming that an axial and a principal ray have been traced, we determine the constant B for use in Eqs. 2.60 and 2.61 which will shift the traced principal ray so that its height at the desired stop surface is zero. This yields B  yp/y where yp and y are taken at the stop surface. Then the new principal ray data at the first surface are New yp  old yp  By New up  old up  Bu The pupil location corresponding to the required stop position is then yp/up, and a principal ray aimed at the center of the pupil will pass through the center of the stop. 2.12 Matrix Optics The form of the paraxial raytracing equations (Eqs. 2.31 and 2.32 or Eqs. 2.41 and 2.42) is A  B  CD. Using Eqs. 2.41 and 2.42, for example, and adding two obvious identities, we have (plus y  y)

u′  u  y

(plus u2  u′1)

y2  y1  du′1

We can write the first set in matrix notation as 1  1

冤 y冥  冤 0

冥 冤 y冥 u

(2.67)

冤 y 冥  冤d1 01冥 冤 y 冥

(2.68)

u′

The second set becomes u2

u′1

2

1

Image Formation (First-Order Optics)

55

Substituting the left side of Eq. 2.67 into Eq. 2.68 and multiplying the two inner matrices, we get 1

冤 y 冥  冤d u2 2

 1  d

冥 冤y 冥 u1 1

which is the matrix form of Eqs. 2.41 and 2.42. This process can be chained to encompass an entire optical system if desired, and the final product of all the inner matrices can be interpreted to yield the cardinal points, focal lengths, etc., of the system. Note well that there is absolutely no magic in this process. The amount of computation involved is exactly the same as in the corresponding paraxial raytrace. To this author it seems far more informative to trace the ray paths and to have the added benefit of a knowledge of the paraxial ray heights and slopes. However, for those to whom matrix manipulation is second nature, this formulation has a definite appeal, although no advantage. 2.13 The y-y bar Diagram The y-ybar diagram is a plot of the ray height y of an axial ray versus the ray height, ybar, of an oblique (i.e., principal or chief) ray. Thus each point on the plot represents a component (or surface) of the system. Figure 2.20a shows an erecting telescope and Fig. 2.20b shows the corresponding y-ybar diagram. Note that point A in the y-ybar diagram corresponds to component A, etc. An experienced practitioner can quickly sketch up a system in y-ybar form in the same way that a system can be sketched using elements and rays. The reduction of either a y-ybar diagram or a sketch with rays to a set of numerical values for the component powers and spacings involves the same amount of computation in either case. Although the y-ybar diagram is simpler to draw than a ray sketch, there is obviously more information in the ray sketch, and an experienced practitioner can easily draw a ray sketch accurately enough to allow conclusions to be drawn as to its practicality, size, etc. which the y  ybar diagram does not readily provide. 2.14 The Scheimpflug Condition To this point we have assumed that the object is defined by a plane surface which is normal to the optical axis. However, if the object plane is tilted with respect to the vertical, then the image plane is also tilted. The Scheimpflug condition is illustrated in Fig. 2.21a, which shows the tilted object and image planes intersecting at the plane of the lens. Or, stated more precisely for a thick lens, the extended object

56

Chapter Two

Figure 2.20 (a) Schematic of an optical system and (b) the corresponding

y-ybar diagram.

and image planes intersect their respective principal planes at the same height. For small tilt angles in the paraxial region, it is apparent from Fig. 2.21a that the object and image tilts are related by s′ ′     m s

(2.69)

where m is the magnification. For finite (real) angles s′ tan ′   tan   m tan  s

(2.70)

Note that in general a tilted object or image plane will cause what is called keystone distortion, because the magnification varies across the field. This results from the variation of object and image distances from top to bottom of the field. This distortion is often seen in overhead projectors when the top mirror is tilted to raise the image projected on the screen. This is equivalent to tilting the screen. As shown in Fig. 2.21b, keystone distortion can be prevented by keeping the plane of the object effectively parallel to the plane of the image. In a projector this means that the field of view of the projection lens must be increased

Image Formation (First-Order Optics)

57

Figure 2.21 (a) The Scheimpflug condition can be used to

determine the tilt of the image surface when the object surface is tilted away from the normal to the optical axis. The magnification under these conditions will vary across the field, producing “keystone” distortion. As diagramed here, the magnification of the top of the object is larger than that of the bottom. (Compare the ratio of image distance to object distance for the rays from the top and bottom of the object.) (b) Keystoning can be avoided if the object and image planes are parallel. The figure shows how the “projection axis” can be tilted upward without producing keystone distortion.

on one side of the axis by the amount that the beam is tilted above the horizontal. 2.15

Summary of Sign Conventions

1. Light travels from left to right. 2. Focal length is positive for converging lenses.

58

Chapter Two

3. Heights above the axis are positive. 4. Distances to the right are positive. 5. A radius or curvature is positive if the center of curvature is to the right of the surface. 6. Angles are positive if the ray is rotated clockwise to reach the normal or the axis. 7. After a reflection (when light direction is reversed), the signs of subsequent indices and spacings are reversed; i.e., if light travels from right to left, the index is negative; if the next surface is to the left, the space is negative. It may be noted that, although the discussions of this chapter have centered about spherical surfaces, and the equations derived have utilized the radii and curvatures of spherical surfaces, the paraxial expressions are equally valid for all surfaces of rotation centered on the optical axis when the osculating radius (i.e., the radius of the surface of the axis) of the surface is used. This includes both conic sections and generalized aspheric surfaces. Bibliography Note: Titles preceded by an asterisk (*) are out of print. Goodman, D. S., “General Principles of Geometric Optics,” in Handbook of Optics, Vol. 1, New York, McGraw-Hill, 1995, Chap. 1. Kingslake, R., Applied Optics and Optical Engineering, Vol. 1: Basic Geometrical Optics, New York, Academic, 1965. Kingslake, R., Optical System Design, New York, Academic, 1983. Smith, W., “Image Formation: Geometrical and, Physical Optics,” in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., “Optical Design” (Chap. 8) and “Optical Elements—Lenses and Mirrors” (Chap. 9), in Wolfe and Zissis (eds.), The Infrared Handbook, Arlington, Va., Office of Naval Research, 1985. Smith, W. J., Practical Optical System Layout, New York, McGrawHill, 1997. Smith, W. J., “Techniques of First-Order Layout,” in Handbook of Optics, Vol. 1, New York, McGraw-Hill, 1995, Chap. 32. Southall, J., Mirrors, Prisms, and Lenses, New York, Dover, 1964. Welford, W., Aberrations of the Symmetrical Optical System, New York, Academic, 1974. Wetherell, W. B., “Afocal Systems,” in Handbook of Optics, Vol. 2, New York, McGraw-Hill, 1995, Chap. 2.

Image Formation (First-Order Optics)

59

Exercises 1 A 10-in-focal-length lens forms an image of a telephone pole which is 200 ft away (from its first principal point). Where is the image located (a) with respect to the focal point of the lens, (b) with respect to the second principal point? ANSWER:

(a) 0.0418 in; (b) 10.0418 in

2 (a) How big is the image (in Exercise 1) if the pole is 50 ft high? (b) What is the magnification? ANSWER:

(a) 2.5104 in; (b) 0.00418

3 A 1-in cube is 20 in away from the first principal point of a negative lens of 5 in focal length. Where is the image and what are its dimensions (height, width, thickness)? ANSWER:

h  0.2 in, w  0.2 in, th  0.04 in. Note that f  5 in.

4 The first principal point of a 2-in-focal-length lens is 1 in from an object. Where is the image and what is the magnification? ANSWER:

s′  2 in, m  2.0

5 A 1-mm detector is “immersed” on the plano surface of a plano convex lens, index 1.5, radius 10 mm. When viewed through the convex surface, where is the image and what is its size if the immersion lens is (a) 7 mm thick, (b) 10 mm thick, (c) 16.67 mm thick? ANSWER: (a) 6.09 mm behind surface and is 1.304  1.304 mm; (b) 10.0 mm behind surface and is 1.5  1.5 mm; (c) 25.0 mm behind surface and is 2.25  2.25 mm

6 Given an equiconvex lens, radii 100, thickness 10, and index 1.5, trace a ray (parallel to the axis) through the lens, beginning at a ray height of (a) 1.0, and (b) 10.0. ANSWER:

y2  0.9667y1

u′2  0.009833y1

7 Determine the effective and back focal lengths of the lens in Exercise 6 (a) from the raytrace data, and (b) using the thick lens equations. ANSWER:

efl  101.6949

bfl  98.3051

8 What is the focal length of the lens in Exercise 6 if it is treated as a thin lens? ANSWER:

100.0

60

Chapter Two

9 A Gregorian telescope objective is composed of a concave primary mirror with a radius of 200 and a concave secondary mirror with a radius of 50. The separation of the two mirrors is 130. Find the effective focal length and locate the focus. Figure 13.38 shows a Gregorian objective. ANSWER:

f  500, bf  150, and focus is 20 behind primary.

10 Find the effective, back, and front focal lengths of a system whose front component has a 10-in focal length and whose rear component has a 10-in focal length when the separation is 5 in. ANSWER:

efl  20; bfl  10; ffl  30

11 What component powers are necessary in a two-element system if one requires a 20-in focal length, a 10-in back focus, and a 5-in air space? ANSWER:

fa  10; fb  10

Chapter

3 Aberrations

3.1

Introduction

In Chap. 2 we discussed the image-forming characteristics of optical systems, but we limited our consideration to an infinitesimal threadlike region about the optical axis called the paraxial region. In this chapter we will consider, in general terms, the behavior of lenses with finite apertures and fields of view. It has been pointed out that wellcorrected optical systems behave nearly according to the rules of paraxial imagery given in Chap. 2. This is another way of stating that a lens without aberrations forms an image of the size and in the location given by the equations for the paraxial or first-order region. We shall measure the aberrations by the amount by which rays miss the paraxial image point. It can be seen that aberrations may be determined by calculating the location of the paraxial image of an object point and then tracing a large number of rays (by the exact trigonometrical ray-tracing equations of Chap. 10) to determine the amounts by which the rays depart from the paraxial image point. Stated this baldly, the mathematical determination of the aberrations of a lens which covered any reasonable field at a real aperture would seem a formidable task, involving an almost infinite amount of labor. However, by classifying the various types of image faults and by understanding the behavior of each type, the work of determining the aberrations of a lens system can be simplified greatly, since only a few rays need be traced to evaluate each aberration; thus the problem assumes more manageable proportions. Seidel investigated and codified the primary aberrations and derived analytical expressions for their determination. For this reason, 61

62

Chapter Three

the primary image defects are usually referred to as the Seidel aberrations. 3.2 The Aberration Polynomial and the Seidel Aberrations With reference to Fig. 3.1, we assume an optical system with symmetry about the optical axis so that every surface is a figure of rotation about the optical axis. Because of this symmetry, we can, without any loss of generality, define the object point as lying on the y axis; its distance from the optical axis is y  h. We define a ray starting from the object point and passing through the system aperture at a point described by its polar coordinates (s, ). The ray intersects the image plane at the point x′, y′. We wish to know the form of the equation which will describe the image plane intersection coordinates y′ and x′ as a function of h, s, and ; the equation will be a power series expansion. While it is impractical to derive an exact expression for other than very simple systems or for more than a few terms of the power series, it is possible to determine the general form of the equation. This is simply because we have assumed an axially symmetrical system. For example, a ray which

Figure 3.1 A ray from the point y  h, (x  0) in the object passes through the opti-

cal system aperture at a point defined by its polar coordinates, (s, ), and intersects the image surface at x′, y′.

Aberrations

63

intersects the axis in object space must also intersect it in image space. Every ray passing through the same axial point in object space and also passing through the same annular zone in the aperture (i.e., with the same value of s) must pass through the same axial point in image space. A ray in front of the meridional (y, z) plane has a mirror-image ray behind the meridional plane which is identical except for the (reversed) signs of x′ and . Similarly, rays originating from ±h in the object and passing through corresponding upper and lower aperture points must have identical x′ intersections and oppositely signed y′ values. With this sort of logic one can derive equations such as the following: y′  A1s cos   A 2h  B 1s3 cos   B2s2h(2  cos 2)  (3B 3  B4)sh2 cos   B5h3  C1s5 cos   (C2  C3 cos 2)s4h  (C4  C6 cos2 )s3h2 cos   (C7  C8 cos 2)s2h3  C10 sh4 cos   C12 h5  D1s7 cos   ...

(3.1)

x′  A1s sin   B1s3 sin   B2s2h sin 2  (B3 B4)sh2 sin   C 1s5 sin   C3s4h sin 2  (C5  C6 cos2 )s3h2 sin   C9s2h3 sin 2  C11sh4 sin   D1s7 sin   ...

(3.2)

where An, Bn, etc., are constants, and h, s, and  have been defined above and in Fig. 3.1. Notice that in the A terms the exponents of s and h are unity. In the B terms the exponents total 3, as in s3, s2h, sh2, and h3. In the C terms the exponents total 5, and in the D terms, 7. These are referred to as the first-order, third-order, and fifth-order terms, etc. There are 2 firstorder terms, 5 third-order, 9 fifth-order, and (n  3) (n  5)   1 8 nth-order terms. In an axially symmetrical system there are no evenorder terms; only odd-order terms may exist (unless we depart from symmetry as, for example, by tilting a surface or introducing a toroidal or other nonsymmetrical surface). It is apparent that the A terms relate to the paraxial (or first-order) imagery discussed in Chap. 2. A2 is simply the magnification (h′/h), and A1 is a transverse measure of the distance from the paraxial focus to our “image plane.” All the other terms in Eqs. 3.1 and 3.2 are called

64

Chapter Three

transverse aberrations. They represent the distance by which the ray misses the ideal image point as described by the paraxial imaging equations of Chap. 2. The B terms are called the third-order, or Seidel, or primary aberrations. B1 is spherical aberration, B2 is coma, B3 is astigmatism, B4 is Petzval, and B5 is distortion. Similarly, the C terms are called the fifthorder or secondary aberrations. C1 is fifth-order spherical aberration; C2 and C3 are linear coma; C4, C5, and C6 are oblique spherical aberration; C7, C8, and C9 are elliptical coma; C10 and C11 are Petzval and astigmatism; and C12 is distortion. The 14 terms in D are the seventh-order or tertiary aberrations; D1 is the seventh-order spherical aberration. A similar expression for OPD, the wave front deformation, is given in Chap. 11. As noted above, the Seidel aberrations of a system in monochromatic light are called spherical aberration, coma, astigmatism, Petzval curvature, and distortion. In this section we will define each aberration and discuss its characteristics, its representation, and its effect on the appearance of the image. Each aberration will be discussed as if it alone were present; obviously in practice one is far more likely to encounter aberrations in combination than singly. The third-order aberrations can be calculated using the methods given in Chap. 10. Spherical aberration

Spherical aberration can be defined as the variation of focus with aperture. Figure 3.2 is a somewhat exaggerated sketch of a simple lens forming an “image” of an axial object point a great distance away. Notice that the rays close to the optical axis come to a focus (intersect the axis) very near the paraxial focus position. As the ray height at the lens increases, the position of the ray intersection with the optical axis moves farther and farther from the paraxial focus. The distance from the paraxial focus to the axial intersection of the ray is called longitudinal spherical aberration. Transverse, or lateral, spherical aberration is the name given to the aberration when it is measured in the “vertical” direction. Thus, in Fig. 3.2 AB is the longitudinal, and AC the transverse spherical aberration of ray R. Since the magnitude of the aberration obviously depends on the height of the ray, it is convenient to specify the particular ray with which a certain amount of aberration is associated. For example, marginal spherical aberration refers to the aberration of the ray through the edge or margin of the lens aperture. It is often written as LAm or TAm. Spherical aberration is determined by tracing a paraxial ray and a trigonometric ray from the same axial object point and determining their final intercept distances l′ and L′. In Fig. 3.2, l′ is distance OA

Aberrations

65

A simple converging lens with undercorrected spherical aberration. The rays farther from the axis are brought to a focus nearer the lens.

Figure 3.2

and L′ (for ray R) is distance OB. The longitudinal spherical aberration of the image point is abbreviated LA′ and LA′  L′  l′

(3.3)

Transverse spherical aberration is related to LA′ by the expression TA′R  LA′ tan U′R  (L′  l′) tan U′R

(3.4)

where U′R is the angle the ray R makes with the axis. Using this sign convention, spherical aberration with a negative sign is called undercorrected spherical, since it is usually associated with simple uncorrected positive elements. Similarly, positive spherical is called overcorrected and is generally associated with diverging elements. The spherical aberration of a system is usually represented graphically. Longitudinal spherical is plotted against the ray height at the lens, as shown in Fig. 3.3a, and transverse spherical is plotted against the final slope of the ray, as shown in Fig. 3.3b. Figure 3.3b is called a ray intercept curve. It is conventional to plot the ray through the top of the lens on the right in a ray intercept plot regardless of the sign convention used for ray slope angles. For a given aperture and focal length, the amount of spherical aberration in a simple lens is a function of object position and the shape, or bending, of the lens. For example, a thin glass lens with its object at infinity has a minimum amount of spherical at a nearly plano-convex shape, with the convex surface toward the object. A meniscus shape, either convex-concave or concave-convex has much more spherical aberration. If the object and image are of equal size (each being two focal lengths from the lens), then the shape which gives the minimum spherical is equiconvex. Usually, a uniform distribution of the amount that a ray is “bent” or deviated will minimize the spherical.

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Figure 3.3 Graphical representation of spherical aberration.

(a) As a longitudinal aberration, in which the longitudinal spherical aberration (LA′) is plotted against ray height (Y). (b) As a transverse aberration, in which the ray intercept height (H′) at the paraxial reference plane is plotted against the final ray slope (tan U′).

The image of a point formed by a lens with spherical aberration is usually a bright dot surrounded by a halo of light; the effect of spherical on an extended image is to soften the contrast of the image and to blur its details. In general, a positive, converging lens or surface will contribute undercorrected spherical aberration to a system, and a negative lens or divergent surface, the reverse, although there are certain exceptions to this. Figure 3.3 illustrated two ways to present spherical aberration, as either a longitudinal or a transverse aberration. Equation 3.4 showed the relation between the two. The same relationship is also appropriate for astigmatism and field curvature (Sec. 3.2.3) and axial chromatic (Sec. 3.3). Note that coma, distortion, and lateral chromatic do not have a longitudinal measure. All of the aberrations can also be expressed as angular aberrations. The angular aberration is simply the angle subtended from the second nodal (or in air, principal) point by the transverse aberration. Thus TA AA   s′

(3.5)

Yet a fourth way to measure an aberration is by OPD, the departure of the actual wave front from a perfect reference sphere centered on the ideal image point, as discussed in Sec. 3.6 and Chap. 11. The transverse measure of an aberration is directly related to the size of the image blur. Graphing it as a ray intercept plot (e.g., Fig. 3.3b and Fig. 3.24) allows the viewer to identify the various types of aberration afflicting the optical system. This is of great value to the

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67

lens designer, and the ray intercept plot of the transverse aberrations is an almost universally used presentation of the aberrations. As discussed later (in Chap. 11), the OPD, or wave-front deformation, is the most useful measure of image quality for well-corrected systems, and a statement of the amount of the OPD is usually accepted as definitive in this regard. The longitudinal presentation of the aberrations is most useful in understanding field curvature and axial chromatic, especially secondary spectrum. Coma

Coma can be defined as the variation of magnification with aperture. Thus, when a bundle of oblique rays is incident on a lens with coma, the rays passing through the edge portions of the lens may be imaged at a different height than those passing through the center portion. In Fig. 3.4, the upper and lower rim rays A and B, respectively, intersect the image plane above the ray P which passes through the center of the lens. The distance from P to the intersection of A and B is called the tangential coma of the lens, and is given by ComaT  H′AB  H′P

(3.6)

where H′AB is the height from the optical axis to the intersection of the upper and lower rim rays, and H′P is the height from the axis to the intersection of the ray P with the plane perpendicular to the axis and passing through the intersection of A and B. The appearance of a point image formed by a comatic lens is indicated in Fig. 3.5. Obviously the aberration is named after the comet shape of the figure. Figure 3.6 indicates the relationship between the position at which the ray passes through the lens aperture and the location which it occupies in the coma patch. Figure 3.6a represents a head-on view of the lens aperture, with ray positions indicated by the letters A through

Figure 3.4 In the presence of coma, the rays through the out-

er portions of the lens focus at a different height than the rays through the center of the lens.

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Figure 3.5 The coma patch. The

image of a point source is spread out into a comet-shaped flare.

Figure 3.6 The relationship between the position of a ray

in the lens aperture and its position in the coma patch. (a) View of the lens aperture with rays indicated by letters. (b) The letters indicate the positions of the corresponding rays in the image figure. Note that the diameters of the circles in the image are proportional to the square of the diameters in the aperture.

H and A′ through D′, with the primed rays in the inner circle. The resultant coma patch is shown in Fig. 3.6b with the ray locations marked with corresponding letters. Notice that the rays which formed a circle on the aperture also form a circle in the coma patch, but as the rays go around the aperture circle once, they go around the image circle twice in accord with the B2 terms in Eqs. 3.1 and 3.2. The primed rays of the smaller circle in the aperture also form a correspondingly smaller circle in the image, and the central ray P is at the point of the figure. Thus the comatic image can be viewed as being made up of a series of different-sized circles arranged tangent to a 60° angle. The size of the image circle is proportional to the square of the diameter of the aperture circle.

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In Fig. 3.6b the distance from P to AB is the tangential coma of Eq. 3.6. The distance from P to CD is called the sagittal coma and is onethird as large as the tangential coma. About half of all the energy in the coma patch is concentrated in the small triangular area between P and CD; thus the sagittal coma is a somewhat better measure of the effective size of the image blur than is the tangential coma. Coma is a particularly disturbing aberration since its flare is nonsymmetrical. Its presence is very detrimental to accurate determination of the image position since it is much more difficult to locate the “center of gravity” of a coma patch than for a circular blur such as that produced by spherical aberration. Coma varies with the shape of the lens element and also with the position of any apertures or diaphragms which limit the bundle of rays forming the image. In an axially symmetrical system there is no coma on the optical axis. The size of the coma patch varies linearly with its distance from the axis. The offense against the Abbe sine condition (OSC) is discussed in Chap. 10. Astigmatism and field curvature

In the preceding section on coma, we introduced the terms “tangential” and “sagittal”; a fuller discussion of these terms is appropriate at this point. If a lens system is represented by a drawing of its axial section, rays which lie in the plane of the drawing are called meridional or tangential rays. Thus rays A, P, and B of Fig. 3.6 are tangential rays. Similarly, the plane through the axis is referred to as the meridional or tangential plane, as may any plane through the axis. Rays which do not lie in a meridional plane are called skew rays. The oblique meridional ray through the center of the aperture of a lens system is called the principal, or chief, ray. If we imagine a plane passing through the chief ray and perpendicular to the meridional plane, then the (skew) rays from the object which lie in this sagittal plane are sagittal rays. Thus in Fig. 3.6 all the rays except A, A′, P, B′, and B are skew rays, and the sagittal rays are C, C′, D′, and D. As shown in Fig. 3.7, the image of a point source formed by an oblique fan of rays in the tangential plane will be a line image; this line, called the tangential image, is perpendicular to the tangential plane; i.e., it lies in the sagittal plane. Conversely, the image formed by the rays of the sagittal fan is a line which lies in the tangential plane. Astigmatism occurs when the tangential and sagittal (sometimes called radial) images do not coincide. In the presence of astigmatism, the image of a point source is not a point, but takes the form of two separate lines as shown in Fig. 3.7. Between the astigmatic foci the image is an elliptical or circular blur. (Note that if diffraction effects are significant, this blur may take on a square or diamond characteristic.)

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Figure 3.7 Astigmatism.

Unless a lens is poorly made, there is no astigmatism when an axial point is imaged. As the imaged point moves further from the axis, the amount of astigmatism gradually increases. Off-axis images seldom lie exactly in a true plane; when there is primary astigmatism in a lens system, the images lie on curved surfaces which are paraboloid in shape. The shape of these image surfaces is indicated for a simple lens in Fig. 3.8. The amount of astigmatism in a lens is a function of the power and shape of the lens and its distance from the aperture or diaphragm which limits the size of the bundle of rays passing through the lens. In the case of a simple lens or mirror whose own diameter limits the size of the ray bundle, the astigmatism is equal to the square of the distance from the axis to the image (i.e., the image height) divided by the focal length of the element, i.e., h2/f. Every optical system has associated with it a sort of basic field curvature, called the Petzval curvature, which is a function of the index of refraction of the lens elements and their surface curvatures. When there is no astigmatism, the sagittal and tangential image surfaces coincide with each other and lie on the Petzval surface. When there is primary astigmatism present, the tangential image surface lies three times as far from the Petzval surface as the sagittal image; note that both image surfaces are on the same side of the Petzval surface, as indicated in Fig. 3.8. When the tangential image is to the left of the sagittal image (and both are to the left of the Petzval surface) the astigmatism is called negative, undercorrected, or inward-(toward the lens) curving. When the

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71

The primary astigmatism of a simple lens. The tangential image is three times as far from the Petzval surface as the sagittal image. Note that the figure is to scale.

Figure 3.8

order is reversed, the astigmatism is overcorrected, or backward-curving. In Fig. 3.8, the astigmatism is undercorrected and all three surfaces are inward-curving. It is possible to have overcorrected (backward curving) Petzval and undercorrected (inward) astigmatism, or vice versa. Positive lenses introduce inward curvature of the Petzval surface to a system, and negative lenses introduce backward curvature. The Petzval curvature (i.e., the longitudinal departure of the Petzval surface from the ideal flat image surface) of a thin simple element is equal to one-half the square of the image height divided by the focal length and index of the element, h2/2nf. Note that “field curvature” means the longitudinal departure of the focal surfaces from the ideal image surface (which is usually flat) and not the reciprocal of the radius of the image surface. Distortion

When the image of an off-axis point is formed farther from the axis or closer to the axis than the image height given by the paraxial expressions of Chap. 2, the image of an extended object is said to be distorted. The amount of distortion is the displacement of the image from the paraxial position, and can be expressed either directly or as a percentage of the ideal image height, which, for an infinitely distant object, is equal to h′  f tan . The amount of distortion ordinarily increases as the image size increases; the distortion itself usually increases as the cube of the image height (percentage distortion increases as the square). Thus, if a centered rectilinear object is imaged by a system afflicted with distortion, it can be seen that the images of the corners will be displaced more (in proportion) than the images of the points making up the sides. Figure 3.9 shows the appearance of a square figure imaged by a

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Figure 3.9 Distortion. (a) Positive,

or pincushion, distortion. (b) Negative, or barrel, distortion. The sides of the image are curved because the amount of distortion varies as the cube of the distance from the axis. Thus, in the case of a square, the cor苶 as much ners are distorted 2兹2 as the center of the sides.

lens system with distortion. In Fig. 3.9a the distortion is such that the images are displaced outward from the correct position, resulting in a flaring or pointing of the corners. This is overcorrected, or pincushion, distortion. In Fig. 3.9b the distortion is of the opposite type and the corners of the square are pulled inward more than the sides; this is negative, or barrel, distortion. A little study of the matter will show that a system which produces distortion of one sign will produce distortion of the opposite sign when object and image are interchanged. Thus a camera lens with barrel distortion will have pincushion distortion if used as a projection lens (i.e., when the film is replaced by a slide). Obviously if the same lens is used both to photograph and to project the slide, the projected image will be rectilinear (free of distortion) since the distortion in the slide will be canceled out upon projection. 3.3 Chromatic Aberrations Because of the fact that the index of refraction varies as a function of the wavelength of light, the properties of optical elements also vary with wavelength. Axial chromatic aberration is the longitudinal variation of focus (or image position) with wavelength. In general, the index of refraction of optical materials is higher for short wavelengths than for long wavelengths; this causes the short wavelengths to be more strongly refracted at each surface of a lens so that in a simple positive lens, for example, the blue light rays are brought to a focus closer to the lens than the red rays. The distance along the axis between the two focus points is the longitudinal axial chromatic aberration. Figure 3.10 shows the chromatic aberration of a simple positive element. When the shortwavelength rays are brought to a focus to the left of the long-wavelength rays, the chromatic is termed undercorrected, or negative. The image of an axial point in the presence of chromatic aberration is a central bright dot surrounded by a halo. The rays of light which are in focus, and those which are nearly in focus, form the bright dot.

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Figure 3.10 The undercorrected longitudinal chromatic aberration of a simple

lens is due to the blue rays undergoing a greater refraction than the red rays.

The out-of-focus rays form the halo. Thus, in an undercorrected visual instrument, the image would have a yellowish dot (formed by the orange, yellow, and green rays) and a purplish halo (due to the red and blue rays). If the screen on which the image is formed is moved toward the lens, the central dot will become blue; if it is moved away, the central dot will become red. When a lens system forms images of different sizes for different wavelengths, or spreads the image of an off-axis point into a rainbow, the difference between the image heights for different colors is called lateral color, or chromatic difference of magnification. In Fig. 3.11 a simple lens with a displaced diaphragm is shown forming an image of an off-axis point. Since the diaphragm limits the rays which reach the lens, the ray bundle from the off-axis point strikes the lens above the axis and is bent downward as well as being brought to a focus. The blue rays are bent downward more than the red and thus form their image nearer the axis. The chromatic variation of index also produces a variation of the monochromatic aberrations discussed in Sec. 3.2. Since each aberration results from the manner in which the rays are bent at the surfaces of the optical system, it is to be expected that, since rays of different color are bent differently, the aberrations will be somewhat different for each color. In general this proves to be the case, and these effects are of practical importance when the basic aberrations are well corrected. 3.4 The Effect of Lens Shape and Stop Position on the Aberrations A consideration of either the thick-lens focal length equation n1 t 1 1 1   (n  1)       n f R1 R2 R1R2

冢

冣

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Figure 3.11 Lateral color, or chromatic difference of magnification,

results in different-sized images for different wavelengths.

or the thin-lens focal length equation 1 1 1   (n  1)     (n  1) (C1  C2) f R1 R2

冢

冣

reveals that for a given index and thickness, there is an infinite number of combinations of R1 and R2 which will produce a given focal length. Thus a lens of some desired power may take on any number of different shapes or “bendings.” The aberrations of the lens are changed markedly as the shape is changed; this effect is the basic tool of optical design. As an illustrative example, we will consider the aberrations of a thin positive lens made of borosilicate crown glass with a focal length of 100 mm and a clear aperture of 100 mm (a speed of f/10) which is to image an infinitely distant object over a field of view of ±17°. A typical borosilicate crown is 517:642, which has an index of 1.517 for the helium d line (  5876 Å), an index of 1.51432 for C light (  6563 Å), and an index of 1.52238 for F light (  4861 Å). (The aberration data presented in the following paragraphs were calculated by means of the thin-lens third-order aberration equations of Chap. 10.) If we first assume that the stop or limiting aperture is in coincidence with the lens, we find that several aberrations do not vary as the lens shape is varied. Axial chromatic aberration is constant at a value of 1.55 mm (undercorrected); thus the blue focus (F light) is 1.55 mm nearer the lens than the red focus (C light). The astigmatism and field curvature are also constant. At the edge of the field (30 mm from the axis) the sagittal focus is 7.5 mm closer to the lens than the paraxial focus, and the tangential focus is 16.5 mm inside the paraxial focus. Two aberrations, distortion and lateral color, are zero when the stop is at the lens.

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75

Spherical aberration and coma, however, vary greatly as the lens shape is changed. Figure 3.12 shows the amount of these two aberrations plotted against the curvature of the first surface of the lens. Notice that coma varies linearly with lens shape, taking a large positive value when the lens is a meniscus with both surfaces concave toward the object. As the lens is bent through plano-convex, convexplano, and convex meniscus shapes, the amount of coma becomes more negative, assuming a zero value near the convex-plano form. The spherical aberration of this lens is always undercorrected; its plot has the shape of a parabola with a vertical axis. Notice that the spherical aberration reaches a minimum (or more accurately, a maximum) value at approximately the same shape for which the coma is zero. This, then, is the shape that one would select if the lens were to be used as a telescope objective to cover a rather small field of view. Note that if both object and image are “real” (i.e., not virtual), the spherical aberration of a positive lens is always negative (undercorrected). Let us now select a particular shape for the lens, say, C1  0.02 and investigate the effect of placing the stop away from the lens, as shown in Fig. 3.13. The spherical and axial chromatic aberrations are

Figure 3.12 Spherical aberration and coma as a function of lens

shape. Data plotted are for a 100-mm focal length lens (with the stop at the lens) at f/10 covering ±17° field.

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The aperture stop away from the lens. Notice that the oblique ray bundle passes through an entirely different part of the lens when the stop is in front of the lens than when it is behind the lens.

Figure 3.13

completely unchanged by shifting the stop, since the axial rays strike the lens in exactly the same manner regardless of where the stop is located. The lateral color and distortion, however, take on positive values when the stop is behind the lens and negative when it is before the lens. Figure 3.14 shows a plot of lateral color, distortion, coma, and tangential field curvature as a function of the stop position. The most pronounced effects of moving the stop are found in the variations of coma and astigmatism. As the stop is moved toward the object, the coma decreases linearly with stop position, and has a zero value when the stop is about 18.5 mm in front of the lens. The astigmatism becomes less negative so that the position of the tangential image approaches the paraxial focal plane. Since astigmatism is a quadratic function of stop position, the tangential field curvature (xt) plots as a parabola. Notice that the parabola has a maximum at the same stop position for which the coma is zero. This is called the natural position of the stop, and for all lenses with undercorrected primary spherical aberration, the natural, or coma-free, stop position produces a more backward curving (or less inward curving) field than any other stop position. Figure 3.12 showed the effect of lens shape with the stop fixed in contact with the lens, and Fig. 3.14 showed the effect of stop position with the lens shape held constant. There is a “natural” stop position for each shape of the simple lens we are considering. In Fig. 3.15, the aberrations of the lens have again been plotted against the lens shape; however, in this figure, the aberration values are those which occur when the stop is in the natural position. Thus, for each bending the coma has been removed by choosing this stop position, and the field is as far backward curving as possible. Notice that the shape which produces minimum spherical aberration also produces the maximum field curvature, so that this shape,

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77

Figure 3.14 Effect of shifting the stop position on the aberrations of a sim-

ple lens. The arrow indicates the “natural” stop position where coma is zero. (efl  100, C1  0.02, speed  f/10, field  ±17°.)

which gives the best image near the axis, is not suitable for wide field coverage. The meniscus shapes at either side of the figure represent a much better choice for a wide field, for although the spherical aberration is much larger at these bendings, the field is much more nearly flat. This is the type of lens used in inexpensive cameras at speeds of f/11 or f/16. 3.5 Aberration Variation with Aperture and Field In the preceding section, we considered the effect of lens shape and aperture position on the aberrations of a simple lens, and in that discussion we assumed that the lens operated at a fixed aperture of f/10 (stop diameter of 10 mm) and covered a fixed field of ±17° (field diameter of 60 mm). It is often useful to know how the aberrations of such a lens vary when the size of the aperture or field is changed. Figure 3.16 lists the relationships between the primary aberrations and the semi-aperture y (in column one) and the image height

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Figure 3.15 The variation of the aberrations with lens shape when the

stop is located in the “natural” (coma free) position for each shape. Data is for 100-mm f/10 lens covering ±17° field, made from BSC-2 glass (517:645).

h (in column two). To illustrate the use of this table, let us assume that we have a lens whose aberrations are known; we wish to determine the size of the aberrations if the aperture diameter is increased by 50 percent and the field coverage reduced by 50 percent. The new y will be 1.5 times the original, and the new h will be 0.5 times the original. Since longitudinal spherical aberration is shown to vary with y2, the 1.5 times increase in aperture will cause the spherical to be (1.5)2, or 2.25, times as large. Similarly transverse spherical, which varies as y3, will be (1.5)3, or 3.375, times larger (as will the image blur due to spherical). Coma varies as y2 and h; thus, the coma will be (1.5)2  0.5, or 1.125, times as large. The Petzval curvature and astigmatism, which vary with h2, will be reduced to (0.5)2, or 0.25, of their previous value, while the blurs due to astigmatism or field curvature will be 1.5(0.5)2, or 0.375, of their original size. The aberrations of a lens also depend on the position of the object and image. A lens which is well corrected for an infinitely distant

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79

Figure 3.16 The variation of the primary aberrations with aperture and field.

object, for example, may be very poorly corrected if used to image a nearby object. This is because the ray paths and incidence angles change as the object position changes. It should be obvious that if all the dimensions of an optical system are scaled up or down, the linear aberrations are also scaled in exactly the same proportion. Thus if the simple lens used as the example in Sec. 3.4 were increased in focal length to 200 mm, its aperture increased to 20 mm, and the field coverage increased to 120 mm, then the aberrations would all be doubled. Note, however, that the speed, or f/number, would remain at f/10 and the angular coverage would remain at ±17 . The percentage distortion would not be changed. Aberrations are occasionally expressed as angular aberrations. For example, the transverse spherical aberration of a system subtends an angle from the second principal point of the system; this angle is the angular spherical aberration. Note that the angular aberrations are not changed by scaling the size of the optical system. 3.6 Optical Path Difference (Wave Front Aberration) Aberrations can also be described in terms of the wave nature of light. In Chap. 1, it was pointed out that the light waves converging to form a “perfect” image would be spherical in shape. Thus when aberrations are present in a lens system, the waves converging on an image point are deformed from the ideal shape (which is a sphere centered on the image point). For example, in the presence of undercorrected spherical aberration the wave front is curled inward at the edges, as shown in Fig. 3.17. This can be understood if we remember that a ray is the path

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Figure 3.17 The optical path difference (OPD) is the dis-

tance between the emerging wave front and a reference sphere (centered in the image plane) which coincides with the wave front at the axis. The OPD is thus the difference between the marginal and axial paths through the system for an axial point.

of a point on the wave front and that the ray is also normal to the wave front. Thus, if the ray is to intersect the axis to the left of the paraxial focus, the section of the wave front associated with the ray must be curled inward. The wave front shown is “ahead” of the reference sphere; the distance by which it is ahead is called the optical path difference, or OPD, and is customarily expressed in units of wavelengths. The wave fronts associated with axial aberrations are symmetrical figures of rotation, in contrast to the off-axis aberrations such as coma and astigmatism. For example, the wave front for astigmatism would be a section of a torus (the outer surface of a doughnut) with different radii in the prime meridians. For off-axis imagery, the reference sphere is chosen to pass through the center of the exit pupil (in some calculations, the reference sphere has an infinite radius, for convenience in computing). 3.7 Aberration Correction and Residuals Section 3.4 indicated two methods which are used to control aberrations in simple optical systems, namely lens shape and stop position. For many applications a higher level of correction is needed, and it is then necessary to combine optical elements with aberrations of opposite signs so that the aberrations contributed to the system by one element are cancelled out, or corrected, by the others. A typical example is the achromatic doublet used for telescope objectives, shown in Fig. 3.18. A single positive element would be afflicted with both undercorrected spherical aberration and undercorrected chromatic aberration. In a negative element, in the other hand, both aberrations are overcorrected. In the doublet a positive element is combined with a less

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81

Figure 3.18 Achromatic doublet

telescope objective. The powers and shapes of the two elements are so arranged that each cancels the aberrations of the other.

powerful negative element in such a way that the aberrations of each balance out. The positive lens is made of a (crown) glass with a low chromatic dispersion, and the negative element of a (flint) glass with a high dispersion. Thus, the negative element has a greater amount of chromatic aberration per unit of power, by virtue of its greater dispersion, than the crown element. The relative powers of the elements are chosen so that the chromatic exactly cancels while the focusing power of the crown element dominates. The situation with regard to spherical aberration is quite analogous except that element power, shape, and index of refraction are involved instead of power and dispersion as in chromatic. If the index of the negative element is higher than the positive, the inner surface is divergent, and will contribute overcorrected spherical to balance the undercorrection of the outer surfaces. Aberration correction usually is exact only for one zone of the aperture of a lens or for one angle of obliquity, because the aberrations of the individual elements do not balance out exactly for all zones and angles. Thus, while the spherical aberration of a lens may be corrected to zero for the rays through the edge of the aperture, the rays through the other zones of the aperture usually do not come to a focus at the paraxial image point. A typical longitudinal spherical aberration plot for a “corrected” lens is shown in Fig. 3.19. Notice that the rays through only one zone of the lens intersect the paraxial focus. Rays through the smaller zones focus nearer the lens system and have undercorrected spherical; rays above the corrected zone show overcorrected spherical. The undercorrected aberration is called residual, or zonal, aberration; Fig. 3.19 would be said to show an undercorrected zonal aberration. This is the usual state of affairs for most optical systems. Occasionally a system is designed with an overcorrected spherical zone, but this is unusual. Chromatic aberration has residuals which take two different forms. The correction of chromatic aberration is accomplished by making the foci of two different wavelengths coincide. However, due to the nature of the great majority of optical materials, the nonlinear dispersion characteristics of the positive and negative elements used in an achromat do not “match up,” so that the focal points of other wavelengths do

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not coincide with the common focal point of the two selected colors. This difference in focal distance is called secondary spectrum. Figure 3.20 shows a plot of back focal distance versus wavelength for a typical achromatic lens, in which the rays for C light (red) and F light (blue) are brought to a common focus. The yellow rays come to a focus about 1/2400th of the focal length ahead of the C-F focal point. The second major chromatic residual may be regarded as a variation of chromatic aberration with ray height, or as a variation of spherical aberration with wavelength, and is called spherochromatism. In ordinary spherochromatism, the spherical aberration in blue light is overcorrected and the spherical in red light is undercorrected (when the spherical aberration for the yellow light is corrected). Figure 3.21 is a spherical aberration plot in three wavelengths for a typical achromatic doublet of large aperture. The correction has been adjusted so that the red and blue rays striking the lens at a height of 0.707 of the marginal ray height are brought to a common focus. The distance between the yellow focus and the red-blue focus at this height is, of course, the

Figure 3.19 Plot of longitudinal

spherical aberration versus ray height for a “corrected” lens. For most lenses, the maximum undercorrection occurs for the ray whose height is 0.707 that of the ray with zero spherical.

Figure 3.20 The secondary spec-

trum of a typical doublet achromat, corrected so that C and F light are joined at a common focus. The distance from the common focus of C and F to the minimum of the curve (in the yellow green at about 0.55 ) is called the secondary spectrum.

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83

Figure 3.21 Spherochromatism. The longitudinal aber-

ration of a “corrected” lens is shown for three wavelengths. The marginal spherical for yellow light is corrected but is overcorrected for blue light and undercorrected for red. The chromatic aberration is corrected at the zone but is overcorrected above it and undercorrected below. A transverse plot of these aberrations is shown in Fig. 3.24k.

secondary spectrum discussed above. Notice that above this 0.707 zone the chromatic is overcorrected and below it is undercorrected so that one half of the area of the lens aperture is overconnected and one half undercorrected. The other aberrations have similar residuals. Coma may be completely corrected for a certain field angle, but will often be overcorrected above this obliquity and undercorrected below it. Coma may also undergo a change of sign with aperture, with the central part of the aperture overcorrected and the outer zone undercorrected. Astigmatism usually varies markedly with field angle. Figure 3.22 shows a plot of the sagittal and tangential field curvatures for a typical photographic anastigmat, in which the astigmatism is zero for one zone of the field. This point is called the node, and typically the two focal surfaces separate quite rapidly beyond the node. 3.8 Ray Intercept Curves and the “Orders” of Aberrations When the image plane intersection heights of a fan of meridional rays are plotted against the slope of the rays as they emerge from the lens, the resultant curve is called a ray intercept curve or an H′–tan U′ curve. The shape of the intercept curve not only indicates the amount of spreading or blurring of the image directly, but also can serve to

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Figure 3.22 Field curvature of a

photographic anastigmat. The astigmatism has been corrected for one zone of the field but is overcorrected inside this zone and undercorrected beyond it.

indicate which aberrations are present. Figure 3.3b, for example, shows simple undercorrected spherical aberration. In Fig. 3.23, an oblique fan of rays from a distant object point is brought to a perfect focus at point P. If the reference plane passes through P, it is apparent that the H′–tan U′ curve will be a straight horizontal line. However, if the reference plane is behind P (as shown) then the ray intercept curve becomes a tilted straight line since the height, H′, decreases as tan U′ decreases. Thus it is apparent that shifting the reference plane (or focusing the system) is equivalent to a rotation of the H′–tan U′ coordinates. A valuable feature of this type of aberration representation is that one can immediately assess the effects of refocusing the optical system by a simple rotation of the abscissa of the figure. Notice that the slope of the line ( H′/ tan U′) is exactly equal to the distance () from the reference plane to the point of focus, so that for an oblique ray fan the tangential field curvature is equal to the slope of the ray intercept curve. The accepted convention for plotting the ray intercepts is that (1) they are plotted for positive image heights (i.e., above the axis) and (2) that the ray through the top of the lens is plotted at the right end of the plot. For compound systems, where the image is relayed by a second component, the ray plotted to the right is the one with the most negative slope, i.e., the one through the bottom of the first component. The result of this is that the sign of the aberrations shown in the ray intercept plot can be instantly recognized. For example, the plot for undercorrected spherical always curves down at the right end and up at the left, and a line connecting the ends of a plot showing positive coma always passes above the point representing the principal ray. Note that in an H′–tan U′ plot, this plotting convention violates the convention for the sign of the ray slope. This seeming contradiction is the result of the change from the historical optical ray slope sign convention which occurred several decades ago.

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85

Figure 3.23 The ray intercept curve (H′ – tan U′) of a point

which does not lie in the reference plane is a tilted straight line. The slope of the line ( H′/ tan U′) is mathematically identical to , the distance from the reference plane to the point of focus P. Note that  is equal to XT, the tangential field curvature, when the paraxial focal plane is chosen as the reference plane.

Figure 3.24 shows a number of intercept curves, each labeled with the aberration represented. The generation of these curves can be readily understood by sketching the ray paths for each aberration and then plotting the intersection height and slope angle for each ray as a point of the curve. Distortion is not shown in Fig. 3.24; it would be represented as a vertical displacement of the curve from the paraxial image height h′. Lateral color would be represented by curves for two colors which were vertically displaced from each other. The ray intercept curves of Fig. 3.24 are generated by tracing a fan of meridional or tangential rays from an object point and plotting their intersection heights versus their slopes. The imagery in the other meridian can be examined by tracing a fan of rays in the sagittal plane (normal to the meridional plane) and plotting their x-coordinate intersection points against their slopes in the sagittal plane (i.e., the slope relative to the principal ray lying in the meridional plane). Note that Fig. 3.24k is for the same lens as the longitudinal plot in Fig. 3.21. It is apparent that the ray intercept curves which are “odd” functions, that is, the curves which have a rotational or point symmetry about the origin, can be represented mathematically by an equation of the form y  a  bx  cx3  dx5  ... or H′  a  b tan U′  c tan3 U′  d tan5 U′  ...

(3.7)

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The ray intercept plots for various aberrations. The ordinate for each curve is H, the height at which the ray intersects the (paraxial) image plane. The abscissa is tan U, the final slope of the ray with respect to the optical axis. Note that it is conventional to plot the ray through the top of the lens at the right of the figure, and that curves for image points above the axis are customarily shown. [Figure continues with parts (d) to (k).]

Figure 3.24

All the ray intercept curves for axial image points are of this type. Since the curve for an axial image must have H′  0 when tan U′  0, it is apparent that the constant a must be a zero. It is also apparent that the constant b for this case represents the amount the reference plane is displaced from the paraxial image plane. Thus the curve for lateral spherical aberration plotted with respect to the paraxial focus can be expressed by the equation TA′  c tan3 U′  d tan5 U′  e tan7 U′  ...

(3.8)

It is, of course, possible to represent the curve by a power series expansion in terms of the final angle U′, or sin U′, or the ray height at the lens (Y ), or even the initial slope of the ray at the object (U0) instead of tan U′. The constants will, of course, be different for each. For simple uncorrected lenses the first term of Eq. 3.8 is usually adequate to describe the aberration. For the great majority of “corrected” lenses the first two terms are dominant; in a few cases

Aberrations

Figure 3.24 (Continued)

87

88

Chapter Three

three terms (and rarely four) are necessary to satisfactorily represent the aberration. As examples, Figs. 3.3, 3.24a, and 3.24b can be represented by TA′  c tan3 U′, and this type of aberration is called thirdorder spherical. Figure 3.24c, however, would require two terms of the expansion to represent it adequately; thus TA′  c tan3 U′  d tan5 U′. The amount of aberration represented by the second term is called the fifth-order aberration. Similarly, the aberration represented by the third term of Eq. 3.8 is called the seventh-order aberration. The fifth-, seventh-, ninth-, etc., order aberrations are collectively referred to as higher-order aberrations. As will be shown in Chap. 10, it is possible to calculate the amount of the primary, or third-order, aberrations without trigonometric raytracing, that is, by means of data from a paraxial raytrace. This type of aberration analysis is called third-order theory. The name “firstorder optics” given to that part of geometrical optics devoted to locating the paraxial image is also derived from this power series expansion, since the first-order term of the expansion results purely from a longitudinal displacement of the reference plane from the paraxial focus. Notes on the interpretation of ray intercept plots

The ray intercept plot is subject to a number of interesting interpretations. It is immediately apparent that the top-to-bottom extent of the plot gives the size of the image blur. Also, a rotation of the horizontal (abscissa) lines of the graph is equivalent to a refocusing of the image and can be used to determine the effect of refocusing on the size of the blur. Figure 3.23 shows that the ray intercept plot for a defocused image is a sloping line. If we consider the slope of the curve at any point on an H–tan U ray intercept plot, the slope is equal to the defocus of a small-diameter bundle of rays centered about a ray represented by that point. In other words, this would represent the focus of the rays passing through a pinhole aperture which was so positioned as to pass the rays at that part of the H–tan U plot. Similarly, since shifting an aperture stop along the axis is, for an oblique bundle of rays, the equivalent of selecting one part or another of the ray intercept plot, one can understand why shifting the stop can change the field curvature, as discussed in Section 3.4. The OPD (optical path difference) or wave-front aberration can be derived from an H–tan U ray intercept plot. The area under the curve between two points is equal to the OPD between the two rays which correspond to the two points. Ordinarily, the reference ray for OPD is either the optical axis or the principal ray (for an oblique bundle).

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89

Thus the OPD for a given ray is usually the area under the ray intercept plot between the center point and the ray. Mathematically speaking, then, the OPD is the integral of the H–tan U plot and the defocus is the first derivative. The coma is related to the curvature or second derivative of the plot, as a glance at Fig. 3.24d will show. It should be apparent that a more general ray intercept plot for a given object point can be considered as a power series expansion of the form H′  h  a  bx  cx2  dx3  ex4  fx5  ...

(3.9)

where h is the paraxial image height, a is the distortion, and x is the aperture variable (e.g., tan U′). Then the art of interpreting a ray intercept plot becomes analogous to decomposing the plot into its various terms. For example, cx2 and ex4 represent third- and fifth-order coma, while dx3 and fx5 are the third- and fifth-order spherical. The bx term is due to a defocusing from the paraxial focus and could be due to curvature of field. Note that the constants a, b, c, etc., will be different for points of differing distances from the axis. For the primary aberrations, the constants will vary according to the table of Fig. 3.16, and in general per Eqs. 3.1 and 3.2. Bibliography Note: Titles preceded by an asterisk are out of print. Smith, W., “Image Formation: Geometrical and Physical Optics” in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., “Optical Design” (Chap. 8) and “Optical Elements—Lenses and Mirrors” (Chap. 9) in W. Wolfe and G. Zissis (eds.), The Infrared Handbook, Arlington, Va., Office of Naval Research, 1985. *Welford, W., Aberrations of the Symmetrical Optical System, New York, Academic, 1974. Exercises 1 The longitudinal spherical aberration of two rays which have been traced through a system is 1.0 and 0.5; the ray slopes (tan U) are 0.5 and 0.35, respectively. What are the transverse aberrations (a) in the paraxial plane, and (b) in a plane 0.2 before the paraxial plane? ANSWER:

(a) 0.5, 0.175; (b) 0.4, 0.105

2 A lens has comaT  1. Plot the focal plane intercepts of 12 rays equally spaced around (a) the marginal zone, (b) the 0.707 zone, and (c) the 0.5 zone (see Fig. 3.6).

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Chapter Three

3 A certain type of lens has the following primary aberrations at a focal length of 100, an aperture of 10, and a field of ±5°: longitudinal spherical  1.0; comaT  1.0; XT  1.0. What are the aberrations of this type of lens when: (a) f  200, aperture  10, field  ±2.50? (b) f  50, aperture  10, field  ±10°? ANSWER:

 2.0

(a) LA  0.5, ComaT  0.25, XT  0.5, (b) LA  2.0, ComaT  4.0, XT

4 Plot the ray intercept curve for a lens with transverse spherical, comaT, and XT, each equal to 1.0. Assume third-order aberrations and also that tan U′m  1.0.

Chapter

4 Prisms and Mirrors

4.1

Introduction

In most optical systems, prisms serve one of two major functions. In spectral instruments (spectroscopes, spectrographs, spectrophotometers, etc.) their function is to disperse the light or radiation; that is, to separate the different wavelengths. In other applications, prisms are used to displace, deviate, or reorient a beam of light or an image. In this type of use, the prism is carefully arranged so that it will not separate the different colors. 4.2 Dispersing Prisms In a typical dispersing prism, as shown in Fig. 4.1, a light ray strikes the first surface at an angle of incidence I1 and is refracted downward, making an angle of refraction I′1 with the normal to the surface. The ray is thus deviated through an angle of (I1  I′1) at this surface. At the second surface the ray is deviated through an angle (I′2  I2), so the total deviation of the ray is given by D  (I1  I′1)  (I′2  I2)

(4.1)

From the geometry of the figure it can be seen that angle I2 is equal to (A  I′1), where A is the vertex angle of the prism; making this substitution in Eq. 4.1, we get D  I1  I′2  A

(4.2)

91

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The deviation of a light ray by a refracting prism. Figure 4.1

To compute the deviation produced by the prism we can readily determine the angles in Eq. 4.2 by Snell’s law (Eq. 1.3) as follows (where n is the prism index): 1 sin I′1   sin I1 (4.3) n (4.4) I2  A  I′1 sin I′2  n sin I2

(4.5)

While it is ordinarily much more convenient to calculate the deviation step by step, using the equations above, it is possible to combine them into a single expression for D, in terms of I1, A, and n as follows: D  I1  A  arcsin [ (n2  sin2 I1)1/2 sin A  cos A sin I1] (4.6) It is apparent that the deviation is a function of the prism index and that the deviation will be increased as the index is raised. For optical materials, the index of refraction is higher for short wavelengths (blue light) than for long wavelengths (red light). Therefore, the deviation angle will be greater for blue light than red, as indicated in Fig. 4.2. This variation of the deviation angle with wavelength is called the dispersion of the prism. An expression for the dispersion can be found by differentiating the preceding equations with respect to the index n, assuming that I1 is constant, yielding, cos I2 tan I′1  sin I2 dD   dn cos I′2

(4.7)

The angular dispersion with respect to wavelength is simply dD/d and is obtained by dividing both sides of Eq. 4.7 by d . The resulting dn/d term on the right is the index dispersion of the prism material. 4.3 The “Thin” Prism If all the angles involved in the prism are very small, we can, as in the paraxial case for lenses, substitute the angle itself for its sine. This case occurs when the prism angle A is small and when the ray is

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93

Figure 4.2 The dispersion of white light into its component

wavelengths by a refracting prism (highly exaggerated).

almost at normal incidence to the prism faces. Under these conditions, we can write i1 i′1   n i1 i2  A  i′1  A   n i′2  ni2  nA  i1 D  i1  i′2  A  i1  nA  i1  A and finally D  A (n  1)

(4.8a)

If the prism angle A is small but the angle of incidence I is not small, we get the following approximate expression for D (which neglects powers of I larger than 3). I 2 (n  1) D  A (n  1) 1    . . . 2n

冤

冥

(4.8b)

These expressions are of great utility in evaluating the effects of a small prismatic error in the construction of an optical system since it allows the resultant deviation of the light beam to be determined quite readily. The dispersion of a “thin” prism is obtained by differentiating Eq. 4.8a with respect to n, which gives dD  Adn. If we substitute A from Eq. 4.8a, we get dn dD  D  (n  1)

(4.9)

Now the fraction (n  1)/ n is one of the basic numbers used to characterize optical materials. It is called the reciprocal relative dispersion,

94

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Abbe V number, or V-value. Ordinarily n is taken as the index for the helium d line (0.5876 m) and n is the index difference between the hydrogen F(0.4861 m) and C(0.6563 m) lines, and the V-value is given by nd  1 V  (4.10) nF  nC Making the substitution of 1/V for dn/(n  1) in Eq. 4.9, we get D dD   (4.11) V which allows us to immediately evaluate the chromatic dispersion produced by a thin prism. 4.4

Minimum Deviation

The deviation of a prism is a function of the initial angle of incidence I1. It can be shown that the deviation is at a minimum when the ray passes symmetrically through the prism. In this case I1  I′2  1⁄2(A  D) and I′1  I2  A/2, so that if we know the prism angle A and the minimum deviation angle D0 it is a simple matter to compute the index of the prism from sin 1⁄2 (A + D0) sin I1 n    sin I′1 sin 1⁄2 A

(4.12)

This is a widely used method for the precise measurement of index, since the minimum deviation position is readily determined on a spectrometer. This position for the prism is also approximated in most spectral instruments because it allows the largest diameter beam to pass through a given prism and also produces the smallest amount of loss due to surface reflections. 4.5 The Achromatic Prism and the Direct Vision Prism It is occasionally useful to produce an angular deviation of a light beam without introducing any chromatic dispersion. This can be done by combining two prisms, one of high-dispersion glass and the other of low-dispersion glass. We desire the sum of their deviations to equal D1,2 and the sum of their dispersions to equal zero. Using the equations for “thin” prisms (Eqs. 4.8 and 4.11), we can express these requirements as follows: Deviation D1,2  D1  D2  A1 (n1  1)  A2 (n2  1)

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95

D1 D2 Dispersion dD1,2  dD1  dD2  0     V1 V2 A2 (n2  1) A1 (n1  1)     V1 V2 A simultaneous solution for the angles of the two prisms gives D1,2V1 A1   (n1  1) (V1  V2)

(4.13)

D1,2V2 A2   (n2  1) (V2  V1) It is apparent that the prism angles will have opposite signs and that the prism with the larger V-value (smaller relative dispersion) will have the larger angle. A sketch of an achromatic prism is shown in Fig. 4.3. Note that the emerging rays are not coincident but are parallel, indicating the same angular deviation. In the direct vision prism it is desired to produce a dispersion without deviating the ray. By setting the deviation D1,2 equal to zero and preserving the dispersion term dD1,2 in the preceding equations we can solve for the angles of two prisms which will produce the desired result. The solution is dD1,2V1V2 A1   (n1  1) (V2  V1)

(4.14)

dD1,2V1V2 A2   (n2  1) (V1  V2) A two-element direct vision prism is shown in Fig. 4.4a. In order to obtain a large enough dispersion for practical purposes it is often necessary to use more than two prisms. Figure 4.4b shows the application of such a prism to a hand spectroscope. Since Eqs. 4.13 and 4.14 were derived using the equations for thin prisms, it is obvious that the values of the component prism angles

Figure 4.3 An achromatic prism. The red and blue rays emerge parallel to each other; no chromatic dispersion is introduced by the deviation.

96

Chapter Four

Figure 4.4 (a) A direct vision prism disperses the light

into its spectral components without deviation of the beam. (b) Hand spectroscope. The collimating lens produces a magnified image of the slit at infinity for easy viewing. The prism then disperses the light into a spectrum without deviation of the yellow ray.

which they give will be approximations to the exact values when the prisms are other than thin. For exact work, these approximate values must be adjusted by exact ray tracing based on Snell’s law. 4.6

Total Internal Reflection

When a light ray passes from a higher index medium to one with a lower index, the ray is refracted away from the normal to the surface as shown in Fig. 4.5a. As the angle of incidence is increased, the angle of refraction increases at a greater rate, in accordance with Snell’s law (n  n′): n sin I′   sin I n′ When the angle of incidence reaches a value such that sin I  n′/n, then sin I′  1.0 and I′  90°. At this point none of the light is transmitted through the surface; the ray is totally reflected back into the denser medium, as is any ray which makes a greater angle to the normal. The angle n′ (4.15) Ic  arcsin  n is called the critical angle and for an ordinary air-glass surface has a value of about 42° if the index of the glass is 1.5; for an index of 1.7, the critical angle is near 36°; for an index of 2.0, 30°; for an index of 4.0, 14.5°.

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97

Figure 4.5 Total internal reflec-

tion occurs when a ray, passing from a higher to a lower index of refraction, has an angle of incidence whose sine equals or exceeds n′/n.

For practical purposes, if the boundary surface is smooth and clean, 100 percent of the energy is redirected along the totally reflected ray. However, it should be noted that the electromagnetic field associated with the light actually does penetrate the surface for a relatively short (to the order of a wavelength) distance. If there is anything near the other side of the boundary surface, the total internal reflection can be “frustrated” to some extent and a portion of the energy will be transmitted. Since the distance of effective penetration is only to the order of the wavelength of the light involved, this phenomenon has been used as the basis of a light valve, or modulator. In the German “LichtSprecher,” an external piece of glass was placed in contact with the reflecting face of a prism to frustrate the reflection, and then moved an extremely short distance away (e.g., a few micrometers) to reinstate the reflection. It should also be noted that the reflection of a totally reflecting surface is decreased by aluminizing or silvering the surface. When this is done, the reflectance drops from 100 percent to the reflectance of the coating applied to the surface. 4.7 Reflection from a Plane Surface Since the prism systems which are discussed in the balance of this chapter are primarily reflecting prisms (the majority of which can be replaced by a system of plane mirrors), we shall first discuss the imaging properties of a plane reflecting surface. Rays originating at an object are reflected according to the law of reflection, which states that both the incident and reflected rays lie in the plane of incidence and that both rays make equal angles with the normal to the surface. The normal to the surface is the perpendicular at the point where the ray strikes the surface, and the plane of incidence is that plane containing the incident ray and the normal.

98

Chapter Four

In Fig. 4.6, the plane of the page is the plane of incidence. Two rays from point P are shown reflected from the surface MM′. By extending the rays backward, it can be seen that after reflection they appear to be coming from point P′, which is a virtual image of point P. Both P and P ′ lie on the same normal to the surface (POP′), and the distance OP is exactly the same as the distance OP′. If we now consider an extended object such as the arrow AB in Fig. 4.7, we can readily locate the position of its image by using the principles of the preceding paragraph to locate the images of points A and B. An observer at E looking directly at the arrow would see the arrowhead A at the top of the arrow. However, in the reflected image, the arrowhead (A′) is at the bottom of the arrow. The image of the arrow has been reoriented (or inverted) by the reflection. If we add a crosspiece CD to the arrow, the image is formed as shown in Fig. 4.8, and although the image of the arrow has been inverted, the image of the crosspiece has the same left-to-right orientation as the object. The preceding discussion has treated reflection from the standpoint of an observer viewing a reflected image. Since the path of light rays is completely reversible, we can equally well consider point P′ in Fig. 4.6 to be an image formed by a lens at the right. Then P would be the reflected image of P ′. Similarly in Figs. 4.7 and 4.8, we may replace the eye with a lens whose image is the primed figure (A′B′ or A′B′C′D′) and view the unprimed figures as their reflected images. A point worth noting is that reflection constitutes a sort of “folding” of the ray paths. In Fig. 4.9, the lens images the arrow at AB. If we now insert reflecting surface MM′, the reflected image is at A′B′. Notice that if the page were folded along MM′, the arrow AB and the solid line rays would exactly coincide with the arrow A′B′ and the reflected (dashed) rays. It is frequently convenient to “unfold” a complex reflecting system; one advantage of this device is that an accurate drawing of the ray paths becomes a simple matter of straight lines.

A plane reflecting surface forms a virtual image of an object point. Object and image are equidistant from the reflecting surface, and both lie on the same normal to the surface.

Figure 4.6

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99

Figure 4.7 The reflected image

A′B′ of the arrow AB appears inverted to an observer at E.

Figure 4.8 The reflected image

is inverted top to bottom, but not left to right.

A useful technique to determine the image orientation after passage through a system of reflectors is to imagine that the image is a transverse arrow, or pencil, which is bounced off the reflecting surface, much as a thrown stick would be bounced off a wall. Figure 4.10 illustrates the technique. The first illustration shows the pencil approaching and striking the reflecting surface, the second shows the point bouncing off the reflector and the blunt end continuing in the original direction, and the third shows the pencil in the new orientation after the reflection. If the process is repeated with the pencil perpendicular to the plane of the paper, the orientation of the other meridian of the image can be determined. The procedure can then be repeated through each reflection in the system.

100

Chapter Four

Figure 4.9 The reflecting surface

MM′ folds the optical system. Note that if the page is folded along MM′, the rays and images coincide.

Figure 4.10 A useful technique

in determining the orientation of a reflected image is to visualize the image as a pencil “bouncing” off a solid wall as it moves along the system axis.

A card marked with the arrow and crossbar of Fig. 4.11 is also useful for this purpose. The reader’s attention is directed to the fact that the initial orientation of the pencil, or pattern, is chosen so that one meridian of the pattern coincides with the plane of incidence. In the majority of reflecting systems, one or the other of the meridians will be in the plane of incidence throughout the system, and the application of this technique is straightforward. Where this is not the case, the card can be marked with a second set of meridians so that the second set is aligned with the plane of incidence. This second set can then be carried through the reflection as before; the orientation of the final image is of course given by the original set of markings. Figure 4.20b exemplifies this method. 4.8 Plane Parallel Plates As will become apparent, most prism systems are the equivalent of a thick block of glass. Thus we continue with a discussion of the effects produced by a plane-parallel plate of glass. Figure 4.12 shows a lens which, in air, would form an image at P. The insertion of the plane parallel plate between the lens and P displaces the image to P ′. If we trace the path of the light rays through the plate, we first notice that the ray emerging from the plate has exactly the same slope angle that it had before passing through the plate, since by Snell’s law, sin I′1  (1/n) sin I1, and I2  I′1 (since the surfaces are parallel). Thus, sin I2  sin I′1  (1/n) sin I1  (1/n) sin I′2, and I1  I′2. Therefore, the effective focal length of the lens system, and the size of the image, are unchanged by the insertion of the plate. The amount of longitudinal displacement of the image is readily determined by application of the paraxial raytracing formulas of Chap. 2, and is equal to (n  1)t/n. The effective thickness of the plate compared to air (the equivalent air thickness) is less than the actual thickness t

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101

Image orientation after reflection.

Figure 4.11

The longitudinal displacement of an image by a plane parallel glass plate. Figure 4.12

by the amount of this shift. The equivalent air thickness is thus found by subtracting the displacement from the thickness and is equal to t/n. The concept of equivalent thickness is useful when one wishes to determine whether a certain size prism can be fitted into the available air space of an optical system, and also in prism system design. If the plate is rotated through an angle I as shown in Fig. 4.13, it can be seen that the “axis ray” is laterally displaced by an amount D, which is given by sin (I  I′) D  t cos I (tan I  tan I′)  t  cos I′ or cos I D  t sin I 1   n cos I′ or 1  sin2 I  D  t sin I 1  n2  sin2 I

冢

冣

冤 冪莦 冥

A power series expansion yields the following expression: tI (n  1) D  n

冤

I 2 (n2  3n  3) 1  6n2

冥

I4 (n4  15n3  15n2  45n  45)  . . .   120n4

102

Chapter Four

Figure 4.13 The lateral displace-

ment of a ray by a tilted plane parallel plate.

For small angles, we can make the usual substitution of the angle for its sine or tangent, or simply use the first term of the expansion to get ti (n  1) d   n This lateral displacement by a tilted plate is used in high-speed cameras (where the rotating plate displaces the image an amount approximately equal to the travel of the continuously moving film) and in optical micrometers. The optical micrometer is usually placed in front of a telescope and used to displace the line of sight. The amount of displacement is read off a calibrated drum connected to the mechanism which tilts the plate. When used in parallel light, a plane parallel plate is free of aberrations (since the rays enter and leave at the same angles). However, if the plate is inserted in a convergent or divergent beam, it does introduce aberrations. The longitudinal image displacement (n  1)t/n is greater for short wavelength light (higher index) than for long, so that overcorrected chromatic aberration is introduced. The amount of displacement is also greater for rays making large angles with the axis; this is, of course, overcorrected spherical aberration. When the plate is tilted, the image formed by the meridional rays is shifted backward while the image formed by the sagittal rays (in a plane perpendicular to the page in the figures) is shifted by a lesser amount, so that astigmatism is introduced. The amount of aberration introduced by a plane parallel plate can be computed by the formulas below. Reference to Fig. 4.14 will indicate the meanings of the symbols U and u—slope angle of the ray to the axis Up and up—the tilt of the plate t—thickness of the plate n—index of the plate V—Abbe V number (nd  1)/(nF  nC)

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103

Figure 4.14

t(n  1) Chromatic aberration  l′F  l′C   n2V n cos U t Spherical aberration  L′  l′   1   2 n 兹n苶  s苶 in2 U

冤

tu2 (n2  1)   2n3

冥

(exact)

(third order)

t Astigmatism  (l′s  l′t )  兹苶 n2  s苶 in2 Up n2 cos2 Up 1   (n2 sin2 Up)

冤

tup2 (n2  1)   n3 tu2up (n2 1) Sagittal coma   2n3 tup(n  1) Lateral chromatic   n2V

冥

(exact)

(third order)

(third order) (third order)

These expressions are extremely useful in estimating the effect that the introduction (or removal) of a plate or a prism system will have on the state of correction of an optical system. A common use for a glass plate is as a beam splitter, tilted at an angle of 45°. In this orientation the astigmatism is approximately a quarter of the thickness of the plate. Since this can severely degrade the image, such plate beam splitters are not recommended in convergent or divergent beams (i.e., where u in Fig. 4.14 is nonzero). Note that the astigmatism can be nullified by inserting another identical

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plate which is tilted in a meridian 90° to the original plate, by introducing either a weak cylinder or a tilted spherical surface, or by wedging the plate. 4.9 The Right-Angle Prism The right-angle prism, with angles of 45°–90°–45°, is the building block of most nondispersing prism systems. Figure 4.15 shows a parallel bundle of rays passing through such a prism, entering through one face, reflecting from the hypotenuse face, and leaving through the second face. If the rays are normally incident on the face of the prism, they are deviated through an angle of 90°. At the hypotenuse face, the rays have an angle of incidence of 45° so that they are subject to total internal reflection. If the entrance and exit faces are low-reflectioncoated, this makes the prism a highly efficient reflector for visual usage since the only losses are the absorption of the material and the reflection losses at the faces which total a few percent or less. (In the ultraviolet and infrared portions of the spectrum, the absorption of a prism may be quite objectionable.) It can be seen that the total internal reflection is limited to rays which have angles of incidence greater than the critical angle, and many prism systems are made of highindex glass to permit total reflection over larger angles. By unfolding the prism, as indicated by the dashed lines in Fig. 4.16, it is apparent that the prism is the equivalent of a glass block with parallel faces, with a thickness equal to the length of the entrance or exit faces. The equivalent air thickness of the block is, of course, this thickness divided by the index of the prism. If the 45°–90°–45° prism is used with the light beam incident on the hypotenuse face as shown in Fig. 4.17, the light is totally reflected twice and the rays emerge in the opposite direction, having been deviated through 180°. Figure 4.17 also indicates the unfolded prism path and the image orientation of this prism. Notice that the image has

Figure 4.15 Right-angle prism.

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Figure 4.16

been inverted, top to bottom, but not left to right. The unfolded prism path is called a tunnel diagram. Such a diagram can be used to determine the angular field of the prism as well as the size of the beam which will pass through the prism. Used in this way, this prism is a constant-deviation prism. Regardless of the angle at which a ray enters the prism, the emergent ray will be parallel, as shown in Fig. 4.18a. This characteristic is a property of the two reflecting surfaces of the prism. A system which directs the light ray back on itself is called a retrodirector; this prism is a retrodirector in one meridian only. (Another of the many constantdeviation systems possible with two reflectors is the 90° deviation arrangement shown in Fig. 4.18b, where the reflecting surfaces are at 45° to each other.) The constant-deviation angle is just twice the angle between the two mirrors. A prism made by cutting off one corner of a cube, so that there are three mutually perpendicular reflecting surfaces, is retrodirective in both meridians. The corner cube (or cube corner) reflector will return all the light rays striking it back toward their source, although the rays will be displaced laterally. A third orientation of the 45°–90°–45° prism is shown in Fig. 4.19, in which the bundle of rays arrives parallel to the hypotenuse face of the prism. After being refracted downward at the entrance face, the rays are reflected upward from the hypotenuse and emerge after a second refraction at the exit face. The unfolded path of the rays (shown in dashed lines) indicates that this prism is the equivalent of a plane parallel plate which is tilted with respect to the axis of the bundle, whereas in the preceding examples the prism faces have been normal to the axis. If this prism is used in a convergent light beam, it will introduce a substantial amount of astigmatism (roughly equal to one-quarter of its thickness). For this reason, this prism, which is known as a Dove prism, is used almost exclusively in parallel light. Since the apex of the prism is not used by the light beam, the prism is usually truncated at AA′. The Dove prism has a very interesting effect on the orientation of the image. In Fig. 4.20a, the arrow and crossbar pattern is shown to be inverted from top to bottom but not left to right. If the prism is

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Right-angle prism used with hypotenuse as entrance and exit face. Figure 4.17

Figure 4.18 (a) The right-angle prism used in the

manner shown is a constant-deviation prism, in that each ray is reflected through exactly 180°. The entering and emergent paths are parallel, regardless of the initial angle the ray makes with the prism. (b) A pair of constant-deviation mirrors. In this case, the deviation produced by the two reflections is always exactly 90°.

Figure 4.19 The Dove prism. The

dashed lines show that the Dove prism is equivalent to a tilted plate and will introduce astigmatism when used in convergent or divergent beams.

rotated 45°, as in Fig. 4.20b, the image is rotated through 90°; if the prism is rotated 90° as in Fig. 4.20c, the pattern is rotated 180°. Thus, the image is rotated twice as fast as the prism. (The analysis of the image orientation in Fig. 4.20b is an example of the use of an auxiliary pattern as described in Sec. 4.7. The auxiliary pattern is shown in dotted lines in Fig. 4.20b.)

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The orientation of an image by a Dove prism. (a) Original position. (b) Prism rotated 45°; image is rotated 90° (c) Prism rotated 90°; image is rotated 180°. Note that the dotted arrow and crossbar in (b) is oriented so that the dotted arrow is in the plane of incidence to simplify the analysis of the image orientation.

Figure 4.20

The length of the Dove prism is four to five times the diameter of the bundle of rays which it will transmit. If two Dove prisms are cemented hypotenuse to hypotenuse (after silvering or aluminizing these faces), the aperture is thereby doubled with no increase in length. The double Dove prism is used in parallel light as is the Dove. It must be precisely fabricated to avoid producing two slightly separated images. When the double Dove is rotated, or tipped, about its center, it can be used as a scanner to change the direction of sight of a telescope or periscope. 4.10

The Roof Prism

If the hypotenuse face of a right-angle prism is replaced by a “roof,” i.e., two surfaces at 90° whose intersection lies in the hypotenuse, the prism is called a roof, or Amici, prism. Face and side views of a roof prism are shown in Fig. 4.21. The addition of the roof to the prism serves to introduce an extra inversion to the image, as can be seen by comparing the final orientation of the cross bar in Fig. 4.11 with that in Fig. 4.22a. This can be understood by tracing the path of the dashed ray in Fig. 4.22a which connects the circles in the arrow and crossbar figures before and after passing through the prism. The angle of incidence (at the roof surface) of the ray shown in Fig. 4.22a is about 60° instead of the 45° it would be for the same ray in the right-angle prism. Even a ray perpendicular to the roof edge has an angle of incidence of 45°. The result is that a roof surface allows total internal reflection for beam angles which would be transmitted through the hypotenuse face of a right-angle prism.

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Figure

prism.

4.21

Roof,

or

Amici,

Figure 4.22 Amici prism (a) showing a single ray path

through the prism and indicating the image orientation, (b) with truncated corners to reduce weight without sacrifice of useful aperture.

In practice, the Amici prism is usually fabricated with the corners cut off, as shown in Fig. 4.22b, in order to reduce the size and weight of the prism. The 90° roof angle must be made to a high order of accuracy. If there is an error in the roof angle, the beam is split into two beams which diverge at an angle which is six times the error. Thus, to avoid any apparent doubling of the image, the roof angle is usually made accurate to one or two seconds of arc. The introduction of a roof degrades the diffraction-limited resolution by a factor approaching 2 in the direction perpendicular to the roof edge (due to a polarization/phase shift on reflection) no matter how perfectly the prism is made. Multilayer coatings have been developed which will reduce this effect. 4.11 Erecting Prism Systems In an ordinary telescope, the objective lens forms an inverted image of the object, which is then viewed through the eyepiece. The image seen by the eye is upside down and reversed from left to right, as indicated in Fig. 4.23. To eliminate the inconvenience of viewing an inverted

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image, an erecting system is often provided to re-invert the image to its proper orientation. This may be a lens system or a prism system. Porro prism of the first type

The most commonly used prism-erecting system is the Porro prism of the first type, illustrated in Fig. 4.24. The Porro system consists of two right-angle prisms oriented at 90° to each other. The first prism inverts the image from top to bottom and the second prism reverses it from left to right. The optical axis is displaced laterally, but is not deviated. One can see that if this system is inserted into the telescope of Fig. 4.23, the final image will have the same orientation as the object. Although the prism system is ordinarily inserted between the objective and eyepiece (to minimize its size), it will erect the image regardless of where it is placed in the system.

In a simple telescope, the objective lens forms a real, inverted internal image of the object, which is reimaged by the eyelens. The image seen by the eye is a virtual inverted image of the object.

Figure 4.23

Figure 4.24 Porro prism system

(first type) (a) indicating the way the Porro system erects an inverted image. (b) Porro prisms are usually fabricated with rounded ends to save space and weight. Note that the spacing between the prisms has been shown increased for clarity.

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The Porro prism (first type) owes its popularity to the fact that the 45°–90°–45° prisms are relatively easy and inexpensive to manufacture, with no critical tolerances. However, if the prisms are not mounted so that their roof edges are exactly at 90° to each other, the final image will be rotated through twice the angular mounting error. This is of special importance in binocular systems where the image presented to one eye must be identical to that presented to the other. A shallow ground slot is often cut across the center of the hypotenuse face of each prism to prevent unwanted grazing angle reflections from this face which originate from outside the field of view. See also Fig. 4.39. Porro prism of the second type

The Porro prism of the second type is shown in Fig. 4.25, and serves the same purpose as the Porro #1 system. Both Porro systems function by total internal reflection so that no silvering is required. It is common to round off the ends of the prisms to conserve space and weight. The second Porro is somewhat more difficult to fabricate than the first type, but in some applications its compactness, and the fact that the prisms can be readily cemented together, offer compensating advantages. The Porro #2 may also be made in three pieces, by cementing two small right-angle prisms on the hypotenuse of a large right-angle prism as indicated in Fig. 4.25b. The lateral displacement of the axis is less than that for the Porro #1 system. Abbe prism

The Abbe (or Koenig, or Brashear-Hastings) prism (Fig. 4.26) is an erecting prism which can be used when it is desired to erect the image

Figure 4.25 Porro prism system (second type) (a) indicating the erection

of an inverted image. This system is shown made from two prisms in (a) and from three prisms in (b).

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Figure 4.26 Abbe prism. Used as

an in-line erecting system, it does not displace the axis as the Porro systems do, nor does it materially displace the image longitudinally.

without displacing the axis as the Porro prisms do. The roof is necessary to provide the left-to-right reversal of the image; the roof angle must be made accurately to avoid image doubling. If this prism is made without the roof, it will invert the image in one meridian only, just as the Dove prism. However, since its entrance and exit faces are normal to the system axis, it may be used in a converging beam without introducing astigmatism. Other erecting prisms

Among the many prisms designed to erect an image are those sketched in Fig. 4.27. The fact that the image is inverted and reversed left to right after passing through these prisms may be verified by the methods outlined in Sec. 4.7. Notice that each prism (except Fig. 4.27f) has been arranged so that the axial ray enters and leaves the prism normal to the prism faces and that all reflections are total internal reflections. In the Leman and Goerz prisms, the axis is displaced but not deviated. In the Schmidt and modified Amici prisms, the axis is deviated through a definite angle, which can be selected by the designer (within the limits allowed by total internal reflection). Note also that the roof surface is used at the location where the angle of incidence is small and where there would be light leakage through an ordinary surface. 4.12

Inversion Prisms

The Dove prism (Figs. 4.19 and 4.20) and the roofless Abbe prism mentioned in Sec. 4.11 are examples of prisms which invert the image in one meridian but not the other. The plane mirror and the right-angle prism (Figs. 4.11 and 4.16) are also simple inversion systems. Figure

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Figure 4.27 Erecting prisms: (a) Schmidt prism; (b) Leman (or Sprenger)

prism; (c) Goerz prism; (d) modified Amici prism; (e) roofed Pechan prism; (f) roofed delta prism.

4.28 shows the above prisms plus the Pechan prism, which is a relatively compact prism for this purpose. Notice that the addition of a “roof” to any of these prism swill convert it to an erecting system. An inversion prism is also known as a derotation prism, since all inversion prisms rotate the image in the same manner as the Dove prism, as shown in Fig. 4.20.

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The mirror version of Fig. 4.28b is called a k-mirror and is useful in infrared and ultraviolet applications where material for a solid prism system is impractical. 4.13

The Penta Prism

The Penta prism (Fig. 4.29a) will neither invert nor reverse the image. Its function is to deviate the line of sight by 90°. It has the valuable property of being a constant-deviation prism, in that it deviates the line of sight through the same angle regardless of its orientation to the line of sight. Most of the prism systems described in this chapter could be replaced by a series of plane mirrors, and this is sometimes done for reasons of weight and/or economy. However, a prism, as a monolithic glass block, is a very stable system and is not as subject to environmental variation of angles as is an assemblage of mirrors on a metal support block.

Inversion (or derotation) prisms: (a) Dove prism; (b) reversion prism; (c) right-angle prism; (d) Pechan prism; (e) delta, or Taylor, prism; (f) compact prism.

Figure 4.28

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Figure 4.29 The Penta prism (a)

and its equivalent mirror system (b).

The Penta prism is used where it is desirable to produce an exact 90° deviation without having to orient the prism precisely. The end reflectors of rangefinders are often of this type, and in optical tooling and precise alignment work, the Penta prism is useful to establish an exact 90° angle. In large rangefinders, however, the prism is replaced by two mirrors (Fig. 4.29b), securely cemented to a block in order to avoid the weight, absorption, and cost of a large block of solid glass. Occasionally a roof is substituted for one of the reflecting faces of the Penta prism to invert the image in one meridian. 4.14

Rhomboids and Beam Splitters

The rhomboid prism is a simple means of displacing the line of sight without affecting the orientation of the image or deviating the line of sight. The rhomboid prism and its mirror system equivalent are shown in Fig. 4.30. A beamsplitter is frequently useful for the purpose of combining two beams (or images) into one, or for separating one beam into two. A thin plate of glass with one surface coated with a semireflecting coating, as shown in Fig. 4.31a, can be used for this purpose, but it suffers from two drawbacks. First, if used in a convergent or divergent beam, it would introduce astigmatism, and second, the reflection from the second surface, although faint, would produce a ghost image displaced from the primary image. (Note that in parallel light neither of these objections is valid, provided the surfaces of the plate are accurately parallel.) The beamsplitter cube (Fig. 4.31b) avoids these difficulties. It is composed of two right-angle prisms cemented together. The hypotenuse of one prism is coated with a semireflecting coating before cementing. Where the weight or absorption of the cube cannot be tolerated, a pellicle is often used as a semireflector. A pellicle is a thin (2- to 10-m) membrane (usually a plastic such as nitrocellulose) stretched over a frame; by virtue of its extreme thinness, both the astigmatism and ghost displacement are reduced to acceptable values.

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Figure 4.30 (a) Rhomboid prism. (b) An equivalent mirror system. Both systems displace the optical axis without deviation or reorientation of the image.

Figure 4.31 Beamsplitters. (a) A thin parallel plate is con-

venient but may be objectionable because of ghosting and astigmatism, unless used in parallel light. (b) Beamsplitting cube has a semireflecting coating supplied to one of the diagonal faces before cementing.

Obviously, the shape of the pellicle surface is determined by the shape of the frame over which it is stretched, and an accurately plane support is necessary. There are two less obvious features of the pellicle which may be disadvantageous: (1) Interference between light reflected from the two surfaces of the extremely thin pellicle can result in a transmission that varies in a rippled way as a function of wavelength, and (2) the pellicle can act as if it were the diaphragm of a microphone, and any atmospheric vibrations can change the shape of the reflecting surface, introducing significant changes in the imagery of the system. This is the basis for one “talk-on-a-beam-of-light” toy. Figure 4.32 shows a prism which is often used in microscope eyepieces to change the direction of the line of sight from vertical to a more-convenient-to-use 45°. As shown, the prism can be used as a beamsplitter either to provide for coaxial illumination or to allow a second eyepiece; without the beamsplitting feature, it simply redirects the line of sight.

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Figure 4.32

In Fig. 4.33, two binocular eyepiece prism systems are sketched. Both serve the same function, namely splitting the light beam from an objective lens into two parts. The two beams are displaced sufficiently so that they can be presented to two eyepieces and both eyes may simultaneously view the same subject. Notice that in both systems, extra glass has been added to the left-hand path so that the amount of glass in each path is identical; in this way the aberrations introduced by the glass are the same for each path. Most of the glass in these systems could be dispensed with if desired, since each of them is equivalent to a beamsplitting cube plus three reflectors. In the system shown in Fig. 4.33b, the two halves can be rotated about the objective axis to vary the spacing between the eyepieces as shown in Fig. 433c. Notice that the image is not rotated by this procedure but retains its original orientation, because the reflecting surfaces are in the form of a rhomboid prism. Often two Porro systems are used in a rotatable configuration which allows a change in the eye separation. 4.15

Plane Mirrors

In the preceding discussions we have indicated several times that reflecting prisms may be replaced by mirrors. For most applications, it is necessary that the mirrors be first-surface mirrors, as opposed to ordinary second-surface mirrors. The two types are sketched in Fig. 4.34. The first-surface mirror is usually preferable because it does not produce a ghost image as does the second-surface mirror. In addition, the second-surface mirror requires the processing of an extra surface in its fabrication. It also requires the light to pass through a thickness of glass which may introduce aberrations and which will absorb energy in ultraviolet and infrared applications. The second-surface mirror can be made more durable, however, since its reflecting coating can be protected from the elements by electrodeposited copper and painted coverings. First-surface mirrors are usually made with vacuumdeposited aluminum films protected by a thin transparent overcoating of silicon monoxide or magnesium fluoride.

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Figure 4.33 Prism systems for binocular eyepiece instruments. System (a) can be

adjusted to match the user’s eye separation by sliding both outer prisms in or out; this defocuses the instrument. Sketch (c) shows how the halves of (b) can be rotated about the objective axis to make this adjustment.

(a) Second-surface mirror. (b) First-surface mirror.

Figure 4.34

4.16 The Design of Prism and Reflector Systems Ordinarily it is required of a prism (or reflector) system that it produce an image with a certain orientation and with the emergent beam of light redirected in a given manner. The design effort is usually best begun by establishing the minimum number of reflectors which will produce the desired result. This is most simply (and perhaps best) accomplished by straightforward trial and error. A rough perspective sketch is made to indicate the reflections necessary to locate the image in its desired position. The orientation of the image is then checked by the technique of Sec. 4.7; reflectors are added in various orientations until the image orientation is correct. Usually several roughly equivalent schemes are possible, and a selection can be made based on the requirements of the application.

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When the reflection system is completed, the optical system is unfolded, i.e., sketched with the optical axis as a straight line. The object, image, and lens apertures are added to the sketch and the necessary sizes for the reflectors are determined in both meridians. If the system is to be composed of prisms, the unfolded layout is repeated with the axial distances adjusted to the “equivalent air thickness” (t/n) for that portion of the system which is glass so that the ray paths can be drawn as straight lines. As an example of reflector system design, let us consider the problem presented by Fig. 4.35. The object at A is to be projected by an ordinary lens B onto a screen at S. The plane of S is parallel to the original projection axis and its center is above the axis by some amount Y. The required orientations of object and image are shown in the sketch. We begin by noting that the image formed by the projection lens will be inverted in both meridians with respect to the object, as shown at C in Fig. 4.35. Now, passing to Fig. 4.36, let us consider the effect of a mirror placed at D. Of the four directions shown as possible reflections at D, the upward reflection labeled D1 seems the most promising since it sends the light in a direction that it must eventually take, so we elect to pursue this line. Using similar reasoning at E, we should be inclined to select E2; however, the image at E2 is rotated 90° from our desired orientation. Selecting E1 on the basis that its image orientation is closest to the desideratum, we consider a reflection at F. Again, F3 is in the proper direction, but the image is reversed from left to right. Case F1 has the proper orientation, but the light is traveling away from the screen. If we add a mirror to reverse the direction of propagation, we will have both orientation and direction as required. To accomplish this without directing the light back through F, we must resort to a figure 4 arrangement as shown in Fig. 4.37, which diagrams the entire system. It is quite apparent that Fig. 4.37 represents only one of the many possible arrangements of mirrors which could be utilized to accomplish

Figure 4.35

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Figure 4.36

Figure 4.37

this same end result. The reader may also have noticed that the discussion has been limited to reflections for which the plane of incidence lay in one of the cartesian reference planes, and also that first consideration was given to reflections which deviated the axis by 90°. For the novice, these restrictions have much to recommend them; one is well advised to keep first trials of this type as simple and uncomplicated as possible. Further, the reduction of the system to practice is much simplified if compound angles are avoided. If our problem had required that the final image be rotated 45°, then we would necessarily have had to depart from the cartesian planes to achieve the desired result. The Porro erecting prism (Fig. 4.38a) will serve as an illustrative example of the “unfolding” technique used in the design of prism systems. The prisms have been unfolded in Fig. 4.38b (for clarity, the second prism is shown rotated 90° about the axis). Each prism can be seen

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to be the equivalent of a glass block whose thickness is twice the size of its end face. Notice that the rays from the lens are refracted at each air-glass surface of the system and that the image has been displaced to the right by the prisms. In Fig. 4.38c, the prisms are drawn with their “equivalent air thickness” as discussed in Section 4.8. This allows us to draw the (paraxial) light rays through the prism as straight lines, simplifying the construction considerably. Now let us suppose that we are to design the minimum size Porro system for a 7  50 binocular. The objective lens has a focal length of 7 in, an aperture of 2 in, and is to cover a 5 8-in-diameter field, as sketched in Fig. 4.39a. We first note that the proportions of face width to “equivalent air thickness” for each prism (Fig. 4.39a) are A:2A/n  1:2/n, or, if we assume an index of 1.50, 3:4. We begin the design from the image and work toward the objective. Placing the exit face of the prism 1 2 in

Figure 4.38 (a) Porro prism system (first type). (b)

Unfolded prisms. Dashed lines indicate path rays would take without prisms. Solid line shows the displacement of the focal point by the prisms. (c) The prisms are drawn to their equivalent air thickness so that the rays can be drawn as straight lines.

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Figure 4.39 The layout of a minimum-size prism system is

shown in (a). The extreme clearance rays connect the rim of the objective with the edge of the field of view. The intersection of the dashed lines (see text) with these rays locates the corner of the smallest prism which will pass the full image cone. In (b) the prisms are drawn to scale, showing their true thickness.

from the image (to allow for clearance and to keep the glass surface well out of the focal plane), we construct the dashed line shown in Fig. 4.39a with a slope of 3:8 (one-half the face-to-equivalent-thickness ratio) starting from the axial intercept of the exit face. This line is, of course, the locus of the corners of a family of prisms of various sizes, and the point where it intersects the extreme clearance ray defines the minimum size prism which will transmit the entire cone of light from the objective. For practical purposes, the prism should be made slightly larger than this to allow for bevels and mounting shoulders. The procedure is now repeated for the other prism; an air space is left between the two to allow for the mounting plate to which both prisms are to be fastened. In Fig. 4.39b, the system is drawn to scale, with the prism blocks expanded to their true length. The reason for the ground slot usually cut into the hypotenuse faces of Porro prisms can be understood from an examination of the unfolded drawings. Light rays from outside the desired field of view can be reflected (by total internal reflection) from these faces back into the field where they are quite annoying; the slot intercepts these rays as they graze along the hypotenuse.

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Figure 4.40 The passage of a ray

through a right-angle prism whose hypotenuse face is tilted from its proper position by a small angle . After reflection, the ray is deviated by 2; this is increased to 3 (or 2n) by refraction at the exit face.

4.17

Analysis of Fabrication Errors

The effects produced by errors in prism angles (due to manufacturing tolerances) are readily analyzed. Such angular errors can be treated as equivalent to the rotation of a reflecting surface from its nominal position, and/or the addition of a thin refracting prism to the system. As an example, consider the right-angle prism shown in Fig. 4.40 and assume that the upper 45° angle is too large by  and that the lower 45° angle is too small by . A ray normal to the entrance face will make an angle of incidence of 45°   at the hypotenuse; the angle of reflection will then be 45°   and the ray will be reflected through an angle of 90°  2. Thus, rotating the reflecting face through  has introduced an error of 2 in the direction of the ray. At the exit face, the ray has an angle of incidence of 2 and, if the prism index is 1.5, an angle of refraction of 3. Thus, the total deviation of the ray from its nominal direction is 3. Also, since the ray has been deviated through an angle  by refraction at this surface, the ray will be dispersed and spread out into a spectrum subtending an angle of /V according to Eq. 4.11. Bibliography Note: Titles preceded by an asterisk are out of print. Hopkins, R. E., in Kingslake (ed.), Applied Optics and Optical Engineering, Vol. 3, New York, Academic, 1966. Hopkins, R. E., Handbook of Optical Design (MIL-HDBK-141), Washington, U.S. Government Printing Office, 1962. Kingslake, R., Applied Optics and Optical Engineering, Vol. 5, New York, Academic, 1969. Kingslake, R., Optical System Design, New York, Academic, 1983.

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Pegis, R., and M. Rao, “Mirror Systems,” Applied Optics, Vol. 2, 1963, Optical Society of America, Washington, D.C., pp. 1271–1274. Smith, W., “Image Formation: Geometrical and Physical Optics,” in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Southall, J., Mirrors, Prisms, and Lenses, New York, Dover, 1964. Walles, S., and R. Hopkins, “Image Orientation” in Applied Optics, Vol. 3, Optical Society of America, Washington, D.C., 1964, pp. 1447–1452. Wolfe, W. L., “Nondispersive Prisms,” in Handbook of Optics, Vol. 2, New York, McGraw-Hill, 1995, Chap. 4. Zissis, G. J., “Dispersive Prisms and Gratings,” in Handbook of Optics, Vol. 2, New York, McGraw-Hill, 1995, Chap. 5.

Chapter

5 The Eye

5.1

Introduction

A knowledge of the characteristics of the human eye is important to the practice of optical engineering because the majority of optical systems utilize the eye as the final element of the system in one way or another. Thus, it is vital that the designer of an optical system understand what the eye can and cannot accomplish. For example, if a visual optical system is required to recognize a certain size target or to measure to a certain degree of accuracy, the magnification of the image presented to the eye must be sufficient to allow the eye to detect the necessary details. On the other hand, it would be wasteful to design a system with a perfection of image rendition which the eye could not utilize. The human eye is a living optical system and its characteristics vary widely from individual to individual. For a given individual, the characteristics may vary from day to day, indeed from hour to hour. Therefore, the data presented in this chapter must be considered as central values in a range of values; in fact, some data are useful only as an indication of the order of magnitude of a certain characteristic. The conditions under which the eye is used play a large role in determining the behavior of the eye and must always be taken into account. In physiological optics, the unit of measure for the power of a lens or optical system is the diopter, the abbreviation for which is D. The diopter power of a lens is simply the reciprocal of its effective focal length, when the focal length is expressed in meters. For example, a lens with a 1-m focal length has a power of 1 diopter; a 1 2-m focal length, 2 diopters; and a lens of 1-in focal length has a power of 40 125

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diopters (or more exactly, 39.37 D). For a single surface, the dioptric power is given by (n′  n)/R, with R the radius in meters. A 1-diopter prism produces a deviation of 1 cm in a 1-m distance, i.e., a deviation of 0.01 radians, or about 0.57 degrees. 5.2 The Structure of the Eye The eyeball is a tough plasticlike shell filled largely with a jellylike substance under sufficient pressure to maintain its shape. It rides in a bony socket of the skull on pads of flesh and fat. It is held in place and rotated by six muscles. Figure 5.1 is a horizontal section of the right eye; the nose is to the left of the figure. The outer shell (sclera) is white and opaque except for the cornea, which is clear. The cornea supplies most (about twothirds) of the refractive power of the eye. Behind the cornea is the aqueous humor, which (as its name implies) is a watery fluid. The iris, which gives the eye its color, is capable of expanding or contracting to control the amount of light admitted to the eye. The pupil formed by the iris can range in diameter from 8 mm in very dim light to less than 2 mm under very bright conditions. The lens of the eye is a flexible capsule suspended by a multitude of fibers, or ligaments, around its periphery. The eye is focused by changing the shape of the lens. When the sphincter muscles to which the suspensory ligaments are connected are relaxed, the lens has its flattest shape and the normal eye is focused at infinity. When these muscles contract, the lens bulges, so that its radii are shorter and the eye is focused for nearby objects. This process is called accommodation. Behind the lens is the vitreous humor, a material with the consistency of thin jelly. All of the optical elements of the eye are largely

Figure 5.1 Schematic horizontal

section of right eyeball (from above).

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water; in fact, a reasonable simulation of the optics of the eye can be made by considering the eye as a single refracting surface of water (nD  1.333, V  55). The following table lists typical values for the radii, thicknesses, and indices of the optical surfaces of the eye. These, of course, vary from individual to individual. R1 (air to cornea)  7.8 mm

t1 (cornea) 0.6

n1 1.376

R2 (cornea to aqueous)  6.4 mm

t2 (aqueous) 3.0

n2 1.336

R3 (aqueous to lens)  10.1 mm

t3 (lens) 4.0

n3 1.386–1.406

R4 (lens to vitreous) 6.1 mm

t4 (vitreous) 16.9

n4 1.337

The principal points are located 1.5 and 1.8 mm behind the cornea, and the nodal points are 7.1 and 7.4 mm behind the cornea. The first focal point is 15.6 mm outside the eye; the second is, of course, at the retina. The distance from the second nodal point to the retina is 17.1 mm; thus the retinal size of an image can be found by multiplying the angular subtense of the object in radians (from the first nodal point) by this distance. When the eye accommodates (focuses), the lens becomes nearly equiconvex with radii of about 5.3 mm, and the nodal points move a few millimeters toward the retina. The center of rotation of the eyeball is 13 to 16 mm behind the cornea. An often overlooked fact is that the commonly accepted eye data tabulated above do not give an adequate picture of the quality of the visual system. First, the surfaces of the eye are not spherical. Some surfaces, especially those of the lens, depart significantly from true spheres. In general, the surface curvature tends to be weaker toward the margin of the surface. Second, the index of the lens is not uniform, but is higher in the central part of the lens. This sort of index gradient produces convergent refracting power in and of itself; it also reduces the surface refracting power at the margin of the lens. Note that both the gradient index and the surface asphericities introduce overcorrected spherical aberration, which offsets the undercorrected spherical of the outer surface of the cornea. The retina contains blood vessels, nerve fibers, the light-sensitive rod and cone cells, and a pigment layer, in that order in the direction that the light travels. The optic nerve and the associated blind spot are located where the nerve fibers leave the eyeball and proceed to the brain. Slightly (about 5°) to the temporal (outer) side of the optical axis of the eye is the macula; the center of the macula is the fovea. At the fovea, the structure of the retina thins out and, in the central 0.3-mm diameter, only cones are present. The fovea is the center of sharp vision. Outside this area rods begin to appear; further away only rods are present.

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There are about 7 million cones in the retina, about 125 million rods, and only about 1 million nerve fibers. The cones of the fovea are 1 to 1.5 m in diameter and are about 2 to 2.5 m apart. The rods are about 2 m in diameter. In the outer portions of the retina, the sensitive cells are more widely spaced and are multiply connected to nerve fibers (several hundred to a fiber), accounting for the less distinct vision in this area of the retina. In the fovea, however, there is one cone cell per fiber. The field of vision of an eye approximates an ellipse about 150° high by about 210° wide. The binocular field of vision, seen by both eyes simultaneously, is approximately circular and about 130° in diameter. 5.3 Characteristics of the Eye

Visual acuity

The characteristic of the eye which is probably of greatest interest to the optical engineer is its ability to recognize small, fine details. Visual acuity (VA) is defined and measured in terms of the angular size of the smallest character that can be recognized. The characters most frequently used to test VA are uppercase letters or a heavy ring with a break in the outline. Many uppercase letters can be considered as made up of five elements; e.g., the letter E has three bars and two spaces. Visual acuity is the reciprocal of the angular size (in minutes of arc) of one of the elements of the letter. “Normal” VA is considered to be 1.0, i.e., when the smallest recognizable letter subtends an angular height of 5 minutes from the eye and each element of the letter subtends 1 minute. Acuity is frequently expressed as the ratio between the distance to the target (usually 20 ft) and the distance at which the target element would subtend 1 minute. Thus, a VA of one-half, or 20/40, indicates that the minimum recognizable letter subtends 10 minutes and its elements 2 minutes. In the Landolt broken ring test, the width of the ring and the width of the break correspond to the letter element size, and recognition consists of determining the orientation of the break. Visual acuity may reach 2 (or 3 in unusual individuals) under ideal conditions. As indicated above, the normal visual acuity is 1 minute, and this is also the value for the angular resolution of the eye which is conventionally assumed in connection with the design of optical instruments. Note that a resolution of one line pair (or one cycle) per minute of arc actually corresponds to a VA of 2, or 20/10. However, this is the value of VA under what might be termed “normal conditions,” and it is the value only for that part of the field of view which corresponds to

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the fovea of the retina. Outside the fovea, the acuity drops rapidly, as indicated in Fig. 5.2, which is a logarithmic plot of visual acuity (relative to that at the fovea, which is arbitrarily set at unity) versus the angular position of the test target in the field of view. Also note that the vertical VA is 5 to 10 percent higher than horizontal and that the horizontal and vertical VA are about 30 percent higher than oblique (45°) VA. As the brightness of a scene is diminished, the iris opens wider and the rods take over from the cones. At low illuminations, the eye is color blind and the fovea becomes a blind spot, since the cones lack the necessary sensitivity to respond to low levels of illumination. One result of this process is that the visual acuity drops as the illumination drops. This relationship is plotted in Fig. 5.3, which also indicates the normal pupil size. Note that the brightness of the area surrounding the test target affects the acuity. A uniform illumination seems to maximize the acuity. Figure 5.4 shows that, as might be expected, reducing the contrast of the target will also reduce the acuity. Because the eye has about 0.75 D of chromatic aberration (C-light to F-light), VA is affected by the wavelength of light illuminating the target. Normally, VA is given for white light. In monochromatic light, the acuity is very slightly higher for the yellow and yellow-green wavelengths and slightly lower for red wavelengths. In blue (or far red) light, VA may be 10 to 20 percent lower, and in violet light the reduction in VA is 20 to 30 percent. The chromatic of the eye can be corrected or doubled

Figure 5.2 The variation of visual acuity (relative to the fovea)

with the retinal position of the image. Note that because of the logarithmic scales of the figure, the falloff in visual acuity is far more rapid than the shape of the curve might indicate.

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Figure 5.3 Visual acuity as a function of object brightness.

Visual acuity in reciprocal minutes. The dashed and dotted lines show the effect of increased and decreased (respectively) surround brightness (1 millilambert is approximately the brightness of a perfect diffuser illuminated by 1 footcandle). The open circle curve indicates the diameter of the pupil; pupil diameters are larger in the young and smaller in the old, especially at lower brightnesses.

Figure 5.4 The object contrast

( B/Bmax) necessary for the eye to resolve a pattern of alternating bright and dark bars of equal width. Note that this curve shifts upward in reduced light levels and drops as the light level is increased. For this plot the bright bars had a brightness of Bmax  23 footlamberts.

(by external lenses) without detection; a quadrupling is noticeable. The effect of the chromatic aberration on the acuity of the eye is less than one might expect because the slightly yellow lens blocks out the ultraviolet, and the macula lutea (which is Latin for yellow spot) filters out the blue and violet light; the spectral response function of the eye is as shown in Fig. 5.8.

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Other types of acuity

Vernier acuity is the ability of the eye to align two objects, such as two straight lines, a line and a cross hair, or a line between two parallel lines. In making settings of this type, the eye is extremely capable. In instrument design, it can be safely assumed that the average person can repeat vernier settings to better than 5 seconds of arc and that he or she will be accurate to about 10 seconds of arc. Exceptional individuals may do as well as 1 or 2 seconds. Thus, the vernier acuity is 5 or 10 times the visual acuity. Vernier acuity is best when setting one line between two, next best setting a line on cross hairs or aligning two butting lines, and less effective in superimposing two lines. The narrowest black line on a bright field that the eye can detect subtends an angle of from 1 2 to 1 second of arc. In conditions of reversed contrast, i.e., a bright line or bright spot, the size of the line is not as important as its brightness. The governing factor is the amount of energy which reaches and triggers the retinal cell into responding. The minimum level seems to be 50 to 100 quanta incident on the cornea (only a few percent of the energy incident on the cornea actually reaches the cell). The eye is capable of detecting angular motion to the order of 10 seconds of arc. The slowest motion that the eye will detect is 1 or 2 minutes of arc per second of time. At the other extreme, a point moving faster than 200° per second will blur into a streak. The eyes judge distance from a number of clues. Accommodation, convergence (the turning in of the eyes to view a near object), haze, perspective, experience, etc., each play a part. Three-dimensional, or stereo, vision results from the separation of the two eyes, which causes each eye to see a slightly different picture of an object. The amount of stereo parallax which can be detected is as small as 2 to 4 seconds. In a clueless surround, a test subject can adjust two rods to be equidistant to within about 1 in when the rods are 20 ft away. The detectable

D in millimeters is approximately the square of the distance in meters (D2). Sensitivity

The lowest level of brightness which can be seen or detected is determined by the light level to which the eye has become accustomed. When the illumination level is reduced, the pupil of the eye expands, admitting more light, and the retina becomes more sensitive (by switching from cone vision to rod vision and also by an electrochemical mechanism involving rhodopsin, the visual purple pigment). This process is called dark adaptation. Figure 5.5 illustrates the adaptation

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The threshold of vision. The minimum brightness perceptible drops sharply with time as the eye adapts itself to darkness. The upper and lower dashed curves show the effect of high and low illumination levels (respectively) before adaptation begins. For areas subtending more than 5° the threshold is almost constant, but rises rapidly as target size is reduced. Curves shown are for a target subtending about 2°.

Figure 5.5

process as a function of the length of time that the eye is in darkness. The “fovea only” curve indicates that after 5 or 10 minutes, the level of brightness detectable by the portion of the retina used for distinct vision is as low as it will ever get. At lower levels of illumination, only the outer portions of the retina are useful; the fovea becomes a blind spot. Figure 5.5 is for a target which subtends about 2°; the threshold brightness is lower for larger targets and higher for smaller targets. As indicated by the dashed lines, the conditions of the test have a great bearing on the threshold of vision, and the data of Fig. 5.5 should be regarded as indicating only an order of magnitude for the threshold. The eye is a poor photometer; it is very inaccurate at judging the absolute level of brightness. However, it is an excellent instrument for comparison purposes, and can be used to match the brightness or color of two adjacent areas with a high degree of precision. Figure 5.6 indicates the brightness difference that the eye can detect as a function of the absolute brightness of the test areas. At ordinary brightness levels, a brightness difference of about 1 or 2 percent is detectable. (Note that in comparison photometry, in which the eye is called upon to match two areas, the precision of setting is increased by making a series of readings. In half the readings, the brightness of the variable area is raised until an apparent match is obtained; in the other half of the readings, the brightness is lowered to obtain the apparent match. The average is then much more accurate than either set.) Contrast sensitivity is best when there is no visible dividing line between the two areas under comparison. When the areas are separated, or if the demarcation between areas is not distinct, contrast sensitivity drops markedly. Figure 5.7 indicates the capability of the normal eye as a comparison colorimeter. Again, the eye is poor at determining the absolute wavelength of a color but quite good at determining a color match;

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Figure 5.6 The contrast sensitivity of the eye as a

function of field brightness. The smallest perceptible difference in brightness between two adjacent fields ( B) as a fraction of the field brightness B remains quite constant for brightnesses above 1 millilambert if the field is large. The dashed line indicates the contrast sensitivity for a dark surrounded field. (One millilambert is approximately the brightness of a perfect diffuser illuminated by one footcandle, i.e., one foot-lambert.)

Figure 5.7 Sensitivity of the eye

to color differences. The amount by which two colors must differ for the difference to be detectable in a side-by-side comparison is plotted as a function of the wavelength. Some data indicates a more uniform sensitivity of about twice that shown here.

wavelength differences of a few millimicrons are detectable under suitable conditions. The comments of the preceding paragraph regarding dividing lines between test areas apply to color sensitivity as well. The sensitivity of the eye to light is a function of the wavelength of the light. Under normal conditions of illumination, the eye is most sensitive to yellow-green light at a wavelength of 0.55 m, and its sensitivity drops off on either side of this peak. For most purposes the sensitivity of the eye may be considered to extend from 0.4 to 0.7 m. Thus, in designing an optical instrument for visual use, the

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monochromatic aberrations are corrected for a wavelength of 0.55 or 0.59 m and chromatic aberration is corrected by bringing the red and blue wavelengths to a common focus. The wavelengths usually chosen are either e(0.5461 m) or d(0.5876 m) for the yellow, C(0.6563 m) for the red, and F(0.4861 m) for the blue. Figure 5.8 shows the sensitivity of the eye as a function of wavelength for normal levels of illumination and also for the dark-adapted eye. The photopic curve applies for brightness levels of 3 cd/m2 or more, and the scotopic curve applies for brightness levels of 3  105 cd/m2 or less. Between these levels, the term “mesopic” is used. Notice that the peak sensitivity for the dark-adapted eye shifts toward the blue end of the spectrum, to a value near 0.51 m. This “Purkinje shift” is due to the differing chromatic sensitivities of the rods and cones of the retina, as shown in Fig. 5.8. Figure 5.9 is a tabulation of the values used in plotting Fig. 5.8. Figure 5.10a is a standardized plot of ocular sensitivity which is used in colorimetry determinations. The long-wavelength portion of this curve (Fig. 5.10b) is useful in estimating the visibility of near-infrared searchlights (as used on sniperscopes, etc.) under conditions where security is desired. 5.4 Defects of the Eye Nearsightedness (myopia) is a defect of focus resulting from too much power in the lens and cornea and/or too long an eyeball. The result is that the image of a distant object falls ahead of the retina and cannot be focused sharply. Since myopia results from an excessive amount of positive power, it can be corrected by placing a negative lens before the eye. The power of the negative lens is chosen so that its image is formed at the most distant point on which the myopic eye can focus. For example, a person with 2 diopters of myopia cannot see clearly beyond 1 2 m (20 in), and a 2 diopter lens (focal length  1 2 m or

Figure 5.8 The relative sensitiv-

ity of the eye to different wavelengths for normal levels of illumination (photopic vision) and under conditions of dark adaptation (scotopic vision).

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Figure 5.9 The standard relative luminosity factors (relative sensitivity or response) for

photopic and scotopic conditions.

20 in) is used to correct for this amount of myopia. The onset of myopia frequently coincides with adolescence, when growth is most rapid. Instrument myopia occurs when an observer (especially an untrained observer) focuses an optical instrument such as a microscope or telescope. There is a tendency to focus the instrument so that the image appears to be about 20 in (2 diopters) away. This may be due to the observer’s perception that the image is inside the instrument and therefore should be nearby. Most experienced observers will focus an instrument much nearer to an infinity setting. They do this by moving the microscope toward the object to focus, so that the image is behind the viewer’s eye (and thus well out of focus) until it is in focus. Instrument myopia may be related to night myopia, where, in the dark and with no stimulus, the eye apparently also focuses at a close distance (60 to 80 in). Farsightedness (hyperopia) is the reverse of myopia and results from too short an eye and/or too little power in the refracting elements of the eye. The image of a distant object is formed (when the eye is relaxed) behind the retina. Hyperopia can be corrected by the use of a positive spectacle lens. Obviously farsighted individuals can, to the extent that their power of accommodation will allow, refocus their eyes

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Figure 5.10 (a) Relative sensitivity of a standardized normal eye to

light of varying wavelengths. (b) Sensitivity in the near-infrared.

to bring the image onto the retina. If prolonged, this may cause headaches. Astigmatism is a difference in the power of the eye from meridian to meridian and usually results from an imperfectly formed cornea, which has a stronger radius in one direction than in the other. Astigmatism of the eye is corrected by the use of toroidal surfaces on the spectacle lenses. A contact lens, placed in contact with the surface of the cornea, effectively changes the curvature of the outer surface of the eye (where most of the visual refractive power occurs). A rigid contact lens can easily correct astigmatism by replacing the toroidal surface of the cornea with its own spherical surface. Obviously, a soft (flexible) contact lens requires an orientation mechanism to align its toroidal power with that of the eye. Myopia and hyperopia can be corrected with contact lenses which flatten or strengthen the curvature of the outer surface of the visual optical system. Radial keratotomy is a surgical technique where radial cuts are made in the cornea (through most of its thickness). This weakens the cornea, and the internal pressure of the eye causes it to bulge in the region of the cuts, thus changing the shape and the power of the cornea. Two obvious drawbacks to this procedure are light scattering from the corneal scars left by the cuts, and the fact that the power of the eye tends to change as one ages, so that the correction may not be permanent. Another technique (PRK) involves a change in corneal shape by sculpting using laser ablation. LASIK slices a thin flap of the

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cornea off and then ablates the cornea to change its shape; the flap is then replaced. The chromatic aberration of the eye was discussed in Sec. 5.3; many eyes have some undercorrected spherical aberration as well. The lens of the eye has aspheric surfaces and a higher index of refraction in the central core of the lens than in the outer portions; both of these factors reduce the power of the system at the margin of the lens and tend to correct the heavy undercorrected spherical from the cornea. A few persons have overcorrected spherical. In most people, the spherical tends toward overcorrection with accommodation, since the lens bulges more at the center than at the edge when the eye focuses on a near point. As much as ±2 diopters of spherical have been measured; however, like chromatic aberration, spherical seems to have little effect on the resolution of the eye. Presbyopia is the inability to accommodate (focus) and results from the hardening of the material of the lens which comes with age. Figure 5.11 indicates the (typical) relationship between age and the power of accommodation. When the eye can no longer accommodate to reading distance (2 or 3 diopters), it is necessary to wear positive lenses to read comfortably. Keratoconus is a conically shaped cornea and can be corrected by contact lenses which effectively overlay a new spherical surface on the cornea. An opaque or cloudy lens (cataract) is frequently removed surgically to restore vision. The resultant loss of power can be made up by an extremely strong positive spectacle lens. But better solutions are a contact lens or by surgically implanting a plastic intraocular lens near

Figure 5.11 The variation of accommodation power

with age (solid line). The dashed line indicates the time in seconds to accommodate to 1.3 diopters.

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the iris. Such an aphakic eye, lacking a lens, cannot accommodate. Also, the change in retinal image size due to the shift in refractive power from inside to outside the eye (if due to the strong spectacle lens) will preclude binocular vision if only one eye is lensless. Aniseikonia is the name given to a disparity in retinal image size from one eye to the other, occurring in otherwise normal eyes, and results in lack of binocular vision if the disparity is larger than a few percent. Aniseikonia can be corrected by special thick meniscus lenses which are effectively low-power telescopes whose magnifications balance out the difference in retinal image size. In instrument design, a number of additional factors should be taken into consideration, especially for binocular instruments. An adjustment must be provided for the variation in interpupillary distance, so that both sides of the instrument can be aligned with the pupils of the eyes. This distance is typically about 21 2 in, but it ranges from 2 to 3 in. Both halves of a binocular instrument must have the same magnification (within 1 2 to 2 percent, depending on the individual’s tolerance) and both halves must have their axes parallel (to within 1 4 prism diopter vertically, 1 2 diopter divergence, and 1 diopter convergence). Each side must be independently focusable to allow for variations in focus between the two eyes. A focus adjustment of ±4 diopters will take care of the requirements of all but a few percent of the population; ±2 diopters will satisfy about 85 percent. The depth of field of the eye (the distance on either side of the point of best focus through which vision is distinct) is about ±1 4 diopter. The Rayleigh quarter wave (see Chap. 11) depth of focus is ±1.1/(pupil diameter)2 diopters, which for a 3-mm pupil works out to ±1 8 diopter. For biocular devices, such as head-up displays (HUDs), the angular disparity between the eyes should be less than 0.001 radians. Bibliography Note: Titles preceded by an asterisk are out of print. *Adler, F., Physiology of the Eye—Clinical Applications, St. Louis, Mosby, 1959. Alpern, M., “The Eyes and Vision,” in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Blaker, W., “Ophthalmic Optics,” in Shannon and Wyant (eds.), Applied Optics and Optical Design, vol. 9, New York, Academic, 1983. Charman, W. N., “Optics of the Eye,” Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 24. *Davson, H., The Physiology of the Eye, London, Blakiston, 1950. Dudley, L., “Stereoscopy,” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 2, New York, Academic, 1965.

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Fry, G., “The Eye and Vision,” in Kingslake (ed.), Applied Optics and Optical Design, vol. 2, New York, Academic, 1965. Geisler, W. S., and M. S. Banks, “Visual Performance,” Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 25. *Hartridge, H., Recent Advances in the Physiology of Vision, London, Blakiston, 1950. Kingslake, R., Optical System Design, New York, Academic, 1983. Lueck, I., “Spectacle Lenses,” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1966. Mouroulis, P., Visual Instrumentation, New York, McGraw-Hill, 1999. Richards, “Visual Optics,” in MIL-HDBK-141, Optical Design, Washington, Defense Supply Agency, 1962. Zoethout, W., Physiological Optics, Professional Press, 1939. Exercises 1 What power telescope is necessary to enable a person with “normal” visual acuity to read letters 1 mm high at a distance of 300 ft? (tangent of 1 minute of arc is 0.0003) ANSWER:

135 

2 What power corrective lens would be prescribed for a nearsighted person who could not focus clearly on an object more than 5 in away? ANSWER:

8 diopters

3 Assuming a depth of focus of ±1 4 diopter, over what range of distance is vision perfectly clear when the eye is focused at 10 in? ANSWER:

11 4 in

4 It is desired to set an optical vernier to a precision of 0.0001 in. Assuming that the vernier projects the image of a ruled scale onto a screen which is viewed from a distance of 10 in and that the setting is made by aligning a scale line with a cross hair on the screen, what magnification must the projection lens of the optical vernier have? Use 10 seconds of arc for the vernier acuity. (Tangent of 1 second is 0.000005) ANSWER:

5 power

5 A convex reflector of radius of curvature  10 in is mounted on a spindle and rotated. (a) What is the largest amount that its center of curvature can be displaced from the axis of rotation without the motion of the reflected image of a distant object being detected by the naked eye? Assume the reflected image is viewed from 10 in. (b) What are the fastest and slowest speeds of rotation at which the motion caused by a decentration of 0.02 in can be detected? ANSWER:

(a) 0.00025 in, (b) 3 to 5 r/min, 300 to 500 r/s

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6 (a) If a plane parallel plate is specified to have zero, ±10 millidiopters, power, what is the shortest tolerable focal length it may have? (b) Assuming one surface is truly flat, what is the strongest (shortest) acceptable radius for the other surface if the index of refraction is 1.6? (c) If the piece has a diameter of 20 mm, how many Newton’s rings will be visible when this surface is tested against a true flat? (Use  0.55 m. One fringe occurs for each /2 change in thickness of the air space.) ANSWER:

(a) ±100 m, (b) ±60 m (c) 3 rings

Chapter

6 Stops and Apertures

6.1

Introduction

In every optical system, there are apertures (or stops) which limit the passage of energy through the system. These apertures are the clear diameters of the lenses and diaphragms in the system. One of these apertures will determine the diameter of the cone of energy which the system will accept from an axial point on the object. This is termed the aperture stop, and its size determines the illumination (irradiance) at the image. Another stop may limit the size or angular extent of the object which the system will image. This is called the field stop. The importance of these stops to the photometry (radiometry) and performance of the system cannot be overemphasized. The elements of an inexpensive camera system are sketched in Fig. 6.1 and illustrate both aperture and field stops in their most basic forms. The diaphragm in front of the lens limits the diameter of the bundle of rays that the system can accept and is thus the aperture stop. The mask adjacent to the film determines the angular field coverage of the system and is quite apparently the field stop of the camera. Not all systems are as obvious as this, however, and we will now consider more complex arrangements. Because the theory of stops is readily explained by the use of a concrete example, the following discussions will be with reference to Fig. 6.2, which is a highly exaggerated sketch of a telescopic system focused on an object at a finite distance. The system shown consists of an objective lens, erector lens, eyelens, and two internal diaphragms. The objective forms an inverted image of the object. This image is then reimaged at the first focal

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The elements of a simple box camera illustrate the functions of elementary aperture and field stops (the diaphragm and mask, respectively).

Figure 6.1

Figure 6.2 Schematic sketch of an optical system to illustrate the relationships between

pupils, stops, and fields.

point of the eyelens by the erector lens, so that the eyelens forms the final image of the object at infinity. 6.2 The Aperture Stop and Pupils By following the path of the axial rays (designated by solid lines) in Fig. 6.2, it can be seen that diaphragm #1 is the aperture of the system which limits the size of the axial cone of energy from the object. All of the other elements of the system are large enough to accept a bigger cone. Thus, diaphragm #1 is the aperture stop of the system. The oblique ray through the center of the aperture stop is called the principal, or chief, ray, and is shown in the figure as a dashed line. The entrance and exit pupils of the system are the images of the aperture stop in object and image space, respectively. That is, the entrance pupil is the image of the aperture stop as it would be seen if viewed from the axial point on the object; the exit pupil is the aperture stop image as it would be seen if viewed from the final image plane (in this case, at an infinite distance). In the system of Fig. 6.2, the entrance pupil lies near the objective lens and the exit pupil lies to the right of the eyelens.

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Notice that the initial and final intersections of the dashed principal ray with the axis locate the pupils, and that the diameter of the axial cone of rays at the pupils indicates the pupil diameters. It can be seen that, for any point on the object, the amount of radiation accepted by, and emitted from, the system is determined by the size and location of the pupils. 6.3

The Field Stop

By following the path of the principal ray in Fig. 6.2, it can be seen that another principal ray starting from a point in the object which is farther from the axis would be prevented from passing through the system by diaphragm #2. Thus, diaphragm #2 is the field stop of this system. The images of the field stop in object and image space are called the entrance and exit windows, respectively. In the system of Fig. 6.2, the entrance window is coincident with the object and the exit window is at infinity (which is coincident with the image). Note that the windows of a system do not coincide with the object and image unless the field stop lies in the plane of a real image formed by the system. The angular field of view is determined by the size of the field stop, and is the angle which the entrance or exit window subtends from the entrance or exit pupil, respectively. The angular field in object space is frequently different from that in image space. (Alternate definition: the angular field of view is the angle subtended by the object or image from the first or second nodal point of the system, respectively. Thus, for nontelescopic systems in air, object and image field angles are equal according to this definition. Note that this definition cannot be applied to an afocal system, which has no nodal or principal points.) 6.4

Vignetting

The optical system of Fig. 6.2 was deliberately chosen as an ideal case in which the roles played by the various elements of the system are definite and clear-cut. This is not usually the situation in real optical systems, since the diaphragms and lens apertures often play dual roles. Consider the system shown in Fig. 6.3, consisting of two positive lenses, A and B. For the axial bundle of rays, the situation is clear; the aperture stop is the clear aperture of lens A, the entrance pupil is at A, and the exit pupil is the image, formed by lens B, of the diameter of lens A. Some distance off the axis, however, the situation is markedly different. The cone of energy accepted from point D is limited on its lower edge by the lower rim of lens A and on its upper edge by the upper rim of lens B. The size of the accepted cone of energy from point D is

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Figure 6.3 Vignetting in a system of separated components. The

cone of rays from point D is limited by the lower rim of lens A and the upper rim of B, and is smaller than the cone accepted from point C. Note that the upper ray from D just passes through the image of lens B which is formed by lens A.

less than it would be if the diameter of lens A were the only limiting agency. This effect is called vignetting, and it causes a reduction in the illumination at the image point D′. It is apparent that for some object point still farther from the axis than point D, no energy at all would pass through the system; thus there is no field stop per se in this system as shown. The appearance of the system when viewed from point D is shown in Fig. 6.4. The entrance pupil has become the common area of two circles, one the clear diameter of lens A, and the other the diameter of lens B as imaged by lens A. The dashed lines in Fig. 6.3 indicate the location and size of this image of B, and the arrows indicate the “effective” aperture stop which has a size, shape, and position completely different than that for the axial case. In a photographic lens with an adjustable iris diaphragm, its location should be such that when stopped down to a small diameter, its clear aperture is centered in the vignetted oblique beam. Example A

Let us determine the pupils, windows, and fields of an optical system of the type shown in Fig. 6.2, assuming the lenses to be “thin lenses.” The elements of the system are as follows: Objective Erector Eyelens:

clear aperture  2.3 in effective focal length  10 in clear aperture  1.7 in effective focal length  2 in clear aperture  1.3 in effective focal length  1 in

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Figure 6.4 The apertures of the optical system of Fig. 6.3 as they are seen from point D.

Diaphragm #1:

clear aperture  0.25 in

Diaphragm #2: clear aperture  0.7 in Distance, object to objective: 50 in Distance, objective to erector: 16.5 in Distance, erector to eyelens: 5 in Distance, erector to diaphragm #1: 2.38 in Distance, erector to diaphragm #2: 4 in We begin the analysis by tracing a paraxial ray from the object point on the axis, using the thin lens raytracing equations (2.41 and 2.42) of Chap. 2. We insert two zero-power elements in the system to represent the diaphragms, so that we can determine the ray heights at the diaphragms. We assume a nominal ray height of 1.0 at the objective lens, giving u1  [1.0/(50.)  0.02. The calculation is shown in the table of Fig. 6.5, lines 3 and 4. To determine which element of the system limits the diameter of the axial cone of rays, we add to our tabulation lines 5 and 6, showing the clear aperture of each element (CA) and the ratio of the clear aperture to the height that the axial ray strikes the element (CA/y).The element for which this ratio is the smallest, in this case diaphragm #1, is the aperture stop. Because of the linear nature of the paraxial equations, we can get the y and u values for any other axial ray by multiplying each entry in lines 3 and 4 by the same constant. If we use for the constant the value of 1 2 CA/y for diaphragm #1 (0.9645), we will get the data for a ray which just passes through the rim of diaphragm #1. This ray data is shown in lines 7 and 8 of the table. A comparison of the new y values of line 7 with the clear apertures of line 5 indicates that the ray will pass through all the other elements with room to spare. To determine the locations of the pupils, we trace a ray through the center of the aperture stop (diaphragm #1) in each direction. The data of such a ray is shown in lines 9 and 10 of the table. We then determine the axial intersections of this ray in object and image space and find that the (apparent) entrance pupil is located 0.1631/0.02474 

146

Figure 6.5

Tabulation of the raytrace data for Example A.

Stops and Apertures

147

6.594 in to the right of the objective lens (note that this differs from Fig. 6.2) and that the exit pupil is 0.566/0.35  1.617 in to the right of the eyelens. The diameter of the pupils is found from the ray data of lines 7 and 8 by determining the ray height in the plane of the pupils. Thus, the diameter of the entrance pupil is 2(0.9645  0.01929  6.594), or 2.183 in, and the diameter of the exit pupil is 2(0.07716  0.0  1.617), or 0.154 in. A comparison of the values of CA/yp would indicate that diaphragm #2 is the field stop. (The ray data in lines 9 and 10 of Fig. 6.5 have already been adjusted so that yp at diaphragm #2 is equal to half of its clear aperture, in a manner analogous to that by which lines 7 and 8 were derived from lines 3 and 4.) The field of view is given by the slope of the principal ray which just skims through the field stop. This is the ray of lines 9 and 10; the object field is ±0.02474 radians and the image field is ±0.35 radians. The linear size of the object field is twice the height at which this ray strikes the object plane, or 2.8 in. A check for vignetting could be made by tracing rays from an object point at the edge of the field through the upper and power rims of the entrance pupil. Again, because of the linearity of the paraxial equations, we can avoid this labor, since the height of the upper rim ray at an element is given by yp  y0 and that of the lower rim ray by yp  y0. (The values of y0 and yp are taken from the ray trace data which has been adjusted, i.e., lines 7 and 9.) This data is tabulated in lines 11 and 12 and a comparison with the clear apertures of the elements indicates that these rays pass through the system without vignetting. An alternate technique for determining the aperture stop is to calculate the size and position of the image of each diameter of the system as seen from the object, i.e., as imaged by all the elements ahead of (or to the left of) the diameter. Then the diameter whose image subtends the smallest angle from the object is the aperture stop. A scale drawing of the images is handy when this technique is used. 6.5 Glare Stops, Cold Stops, and Baffles A glare stop is essentially an auxiliary diaphragm located at an image of the aperture stop for the purpose of blocking out stray radiation. Depending on the system application, a glare stop may be called a Lyot stop, or in an infrared system, a cold stop. Figure 6.6 shows an erecting telescope in which the primary aperture stop is at the objective lens. Energy from sources outside the desired field of view, passing through the objective and reflecting from an internal wall, shield, or supporting member, can create a glare which reduces the contrast of the image formed by the system. In a long wavelength infrared

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Figure 6.6 Stray light reflected from an inside wall of the telescope, is intercepted

by the glare stop, which is located at the internal image of the objective lens.

system, the housing itself may be a source of unwanted thermal radiation. This radiation can be blocked out by an internal diaphragm which is an accurate image of the objective aperture. This stop is usually cooled and is located inside the evacuated detector Dewar. Since the stray radiation will appear to be coming from the wall, and thus from outside the objective aperture, it will be imaged on the opaque portion of the diaphragm. Another glare stop could conceivably be located at the exit pupil of this particular system, since it is real and accessible; however, it would make visual use of the instrument quite inconvenient. In most systems the aperture stop is located at or very near the objective lens. This location gives the smallest possible diameter for the objective, and since the objective is usually the most expensive component (per inch of diameter), minimizing its diameter makes good economic sense. In addition, there are often aberration considerations which make this a desirable location. However, there are some systems, such as scanners, where the need to minimize the size and weight of the scanner mirror makes it necessary to put the stop or pupil at the scanner mirror rather than at the objective. This causes the objective to be larger, more costly, and more difficult to design. In an analogous manner, field stops could be placed at both internal images to further reduce stray radiation. The principle here is straightforward. Once the primary field and aperture stops of a system are determined, auxiliary stops may be located at images of the primary stops to cut out glare. If the glare stops are accurately located and are the same size as the images of the primary stops (or slightly larger), they do not reduce the field or illumination, nor do they introduce vignetting. Baffles are often used to reduce the amount of radiation that is reflected from walls, etc., in a system. Figure 6.7 shows a simple radiometer consisting of a collector lens and a detector in a housing. Assume that radiation from a powerful source (such as the sun) outside the field of view reflects from the inner walls of the mount onto the detector and obscures the measurement of radiation from the

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149

desired target, as shown in the upper half of the sketch. Under these conditions, there is no possibility of using an internal glare stop (since there is no internal image of the entrance pupil) and the internal walls of the mount must be baffled as shown in the lower half of the sketch (although an eternal hood or sunshade could also be used if circumstances permit). The key to the efficient use of baffles is to arrange them so that no part of the detector can “see” a surface which is directly illuminated. The method of laying out a set of baffles is illustrated in Fig. 6.8. The dotted lines from the rim of the lens to the edge of the detector indicate the necessary clearance space, into which the baffles cannot intrude without obstructing part of the radiation from the desired field

Figure 6.7 Stray (undesired) radiation from outside the use-

ful field of this simple radiometer can be reflected from the inner walls of the housing and degrade the function of the system. Sharp-edged baffles, shown in the lower portion, trap this radiation and prevent the detector from “seeing” a directly illuminated surface.

Figure 6.8 Construction for the systematic layout of baf-

fles. Note that baffle #3 shields the wall back to point D; thus, all three baffles could be shifted forward somewhat, so that their coverages overlap.

150

Chapter Six

of view. The dashed line AA′ is a “line of sight” from the detector to the point on the wall where the extraneous radiation begins. The first baffle is erected to the intersection of AA′ with the dotted clearance line. Solid line BB′ indicates the path of stray light from the top of the lens to the wall. The area from Baffle #1 to B′ is thus shadowed and “safe” for the detector to “see.” The dashed line from B′ to A is thus the safe line of sight, and baffle #2 at the intersection of AB′ and the clearance line will prevent the detector from “seeing” the illuminated wall beyond B′. This procedure is repeated until the entire side wall is protected. Note that the inside edges of the baffles should be sharp and their surfaces rough and blackened. The cast and machined baffles shown in Fig. 6.7 are obviously expensive to fabricate. Less expensive alternatives include washers constrained between spacers, or stamped, cup-shaped washers which can be cemented or press-fitted into place. This type of baffling is not necessary in all cases. Frequently, internal scattering can be sufficiently reduced by scoring or threading the offending internal surfaces of the mount. In this way, the reflections are broken up and scattered, reducing the amount of reflection and destroying any glare images. The use of a flat black paint is also highly advisable, although care must be taken to be sure that the paint remains both matte and black at near-grazing angles of incidence and at the application wavelength. Sandblasting to roughen the surface and blackening (for aluminum, black anodizing works well) is a simple and usually effective treatment. Another treatment is the application of black “flocked” paper. This can be procured in rolls, cut to size, and cemented to the offending surfaces; this is especially useful for large internal surfaces and for laboratory equipment. Specialized flat black paints are available for specific applications and wavelengths. In the absence of special paints, Floquil brand flat black model locomotive paint usually can be found at the local hobby shop and makes a pretty good general-purpose flat black. A specialized anodizing process, Martin Optical Black (or Martin Infrablack for the infrared) is extremely effective (0.2 percent reflective) but is very fragile. 6.6 The Telecentric Stop A telecentric system is one in which the entrance pupil and/or the exit pupil is located at infinity. A telecentric stop is an aperture stop which is located at a focal point of an optical system. It is widely utilized in optical systems designed for metrology (e.g., comparators and contour projectors and in microlithography) because it tends to reduce the measurement or position error caused by a slight defocusing of the

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151

system. Figure 6.9a shows a schematic telecentric system. Note that the dashed principal ray is parallel to the axis to the left of the lens. If this system is used to project an image of a scale (or some other object), it can be seen that a small defocusing displacement of the scale does not change the height on the scale at which the principal ray strikes, although it will, of course, blur the image. Contrast this with Fig. 6.9b where the stop is at the lens, and the defocusing causes a proportional error in the ray height. The telecentric stop is also used where it is desired to project the image of an object with depth (along the axis), since it yields less confusing images of the edges of such an object. 6.7 Apertures and Image Illumination— f-Number and Cosine-Fourth

f-Number

When a lens forms the image of an extended object, the amount of energy collected from a small area of the object is directly proportional to the area of the clear aperture, or entrance pupil, of the lens. At the image, the illumination (power per unit area) is inversely proportional to the image area over which this object is spread. Now the aperture area is proportional to the square of the pupil diameter, and the image area is proportional to the square of the image distance, or focal

Figure 6.9 The telecentric stop is located at the focal point

of the projection system shown, so that the principal ray is parallel to the axis at the object. When the object is slightly out of focus (dotted) there is no error in the size of the projected image as there is in the system with the stop at the lens, shown in the lower sketch.

152

Chapter Six

length. Thus, the square of the ratio of these two dimensions is a measure of the relative illumination produced in the image. The ratio of the focal length to the clear aperture of a lens system is called the relative aperture, f-number, or “speed” of the system, and (other factors being equal), the illumination in an image is inversely proportional to the square of this ratio. The relative aperture is given by: f-number  efl/clear aperture

(6.1)

As an example, an 8-in focal length lens with a 1-in clear aperture has an f-number of 8; this is customarily written f/8 or f:8. Another way of expressing this relationship is by the numerical aperture (usually abbreviated as N.A. or NA), which is the index of refraction (of the medium in which the image lies) times the sine of the half angle of the cone of illumination. Numerical aperture  NA  n′ sin U′

(6.2)

Numerical aperture and f-number are obviously two methods of defining the same characteristic of a system. Numerical aperture is more conveniently used for systems that work at finite conjugates (such as microscope objectives), and the f-number is appropriately applied to systems for use with distant objects (such as camera lenses and telescope objectives). For aplanatic systems (i.e., systems corrected for coma and spherical aberration) with infinite object distances, the two quantities are related by: 1 f-number   (6.3) 2NA The terms “fast” and “slow” are often applied to the f-number of an optical system to describe its “speed.” A lens with a large aperture (and thus a small f-number) is said to be “fast,” or to have a high “speed.” A smaller aperture lens is described as “slow.” This terminology derives from photographic usage, where a larger aperture allows a shorter (or faster) exposure time to get the same quantity of energy on the film and may allow a rapidly moving object to be photographed without blurring. It should be apparent that a system working at finite conjugates will have an object-side numerical aperture as well as an image-side numerical aperture and that the ratio NA/NA′  (object-side NA)/(image-side NA) must equal the absolute value of the magnification. The term “working f-number” is sometimes used to describe the numerical aperture in f-number terms. If we use the terms “infinity f-number” for the f-number defined in Eq. 6.1, then the image-side

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153

working f-number is equal to the infinity f-number times (1  m), where m is the magnification. Another term that is occasionally encountered is the T-stop, or T-number. This is analogous to the f-number, except that it takes into account the transmission of the lens. Since an uncoated, manyelement lens made of exotic glass may transmit only a fraction of the light that a low-reflection coated lens of simpler construction will transmit, such a speed rating is of considerable value to the photographer. The relationship between f-number, T-number, and transmission is f-number T-number   兹苶 transm苶 ission

(6.4)

Cosine-to-the-fourth

For off-axis image points, even when there is no vignetting, the illumination is usually lower than for the image point on the axis. Figure 6.10 is a schematic drawing showing the relationship between exit pupil and image plane for point A on axis and point H off axis. The illumination at an image point is proportional to the solid angle which the exit pupil subtends from the point. The solid angle subtended by the pupil from point A is the area of the exit pupil divided by the square of the distance OA. From point H, the solid angle is the projected area of the pupil divided by the square of the distance OH. Since OH is greater than OA by a factor equal to 1/cos , this increased distance reduces the illumination by a factor of cos2 . The exit pupil is viewed obliquely from point H, and its projected area is reduced by a factor which is approximately cos . (This is a fair approximation if OH is large compared to the size of the pupil; for high-speed lenses used at large obliquities, it may be subject to significant errors. See Example A in Chap. 8 for an exact expression.) Thus the illumination at point H is reduced by a factor of cos3 . This is, however, true for illumination on a plane normal to the line OH

Figure 6.10 Relationship between

exit pupil and image points, used to demonstrate that the illumination at H is cos4  times that at A.

154

Chapter Six

(indicated by the dashed line in Fig. 6.10). We want the illumination in the plane AH. An illumination of x lumens per square foot on the dashed plane will be reduced on plane AH because the same number of lumens is spread over a greater area in plane AH. The reduction factor is cos , and combining all the factors we find that Illumination at H  cos4  (illumination at A)

(6.5)

The importance of this effect on wide-angle lenses can be judged from the fact that cos4 30°  0.56, cos4 45°  0.25, and cos4 60°  0.06. It can be seen that the illumination on the film in a wide-angle camera will fall off quite rapidly. Note that the preceding has been based on the assumption that the pupil diameter is constant (with respect to ) and that  is the angle formed in image space (although many people apply it to the field angle in object space). The “cosine fourth law” can be modified if the construction of the lens is such that the apparent size of the pupil increases for off-axis points, or if a sufficiently large amount of barrel distortion is introduced to hold  to smaller values than one would expect from the corresponding field angle in object space. Certain extreme wide-angle camera lenses make use of these principles to increase off-axis illumination. The cos4 effect is in addition to any illumination reduction caused by vignetting. It should be remembered that the cosine-fourth effect is not a “law” but a collection of four cosine factors which may or may not be present in a given situation. 6.8

Depth of Focus

The concept of depth of focus rests on the assumption that for a given optical system, there exists a blur (due to defocusing) of small enough size such that it will not adversely affect the performance of the system. The depth of focus is the amount by which the image may be shifted longitudinally with respect to some reference plane (e.g., film, reticle) and which will introduce no more than the acceptable blur. The depth of field is the amount by which the object may be shifted before the acceptable blur is produced. The size of the acceptable blur may be specified as the linear diameter of the blur spot (as is common in photographic applications) (Fig. 6.11) or as an angular blur, i.e., the angular subtense of the blur spot from the lens. Thus, the linear and angular blurs (B and , respectively and the distance D are related by B′ B     D D′

(6.6)

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155

Figure 6.11 When an optical sys-

tem is defocused, the image of a point becomes a blurred spot. The size of the blur is determined by the relative aperture of the system and the focus shift.

for a system in air, where the primed symbols refer to the image-side quantities. Angular depth of focus

From Fig. 6.12, it can be seen that the depth of field  for a system with a clear aperture A can be obtained from the relationship  D     (D ± ) A This expression can be solved for the depth of field, giving D2 DB     (A ± D) (A ± B)

(6.7)

Note that the depth of field toward the optical system is smaller than that away from the system. When  is small in comparison with the distance D, this reduces to D D2     (6.8) A A For the image side, the relationship is F 2 D′2 ′      F (f/#)  B′(f/#) (6.9) A A where the second, third, and fourth forms of the right-hand side apply when the image is at the focal point of the system, and F is the system focal length. The depth of focus in terms of linear blur-spot size B can be obtained by substituting Eq. 6.6 into the above. Also, note that the depth of field  and the depth of focus ′ are related by the longitudinal magnification of the system, so that

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Figure 6.12 Relationships used

to determine the longitudinal depth of field in terms of a tolerable angular blur.

′  苶 m ⬇ m2

(6.10)

The hyperfocal distance of a system is the distance at which the system must be focused so that the depth of field extends to infinity. If (D  ) equals infinity, then ß is equal to A/D, so that F

A D (hyperfocal)     B 

(6.11)

The photographic depth of focus

The photographic depth of focus is based on the concept that a defocus blur which is smaller than a silver grain in the film emulsion will not be noticeable. This concept also can be applied to pixel size in, for example, a charge-coupled device (CCD). If the acceptable blur diameter is B, then the depth of focus (at the image) is simply ′  ± B(f-number) B ′  ±  2NA

(6.12)

The corresponding depth of field (at the object) is from Dnear to Dfar, where fD (A  B) Dnear   (fA  DB)

(6.13)

fD (A  B) Dfar   (fA  DB)

(6.14)

and the hyperfocal distance is simply fA Dhyp   B

(6.15)

where D  the nominal distance at which the system is focused (note that, by our sign convention, D is normally negative)

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157

A  the diameter of the entrance pupil of the lens f  the focal length of the lens Note that there are several false assumptions here. We assume that the image is a perfect point, with no diffraction effects. We also assume that the lens has no aberrations and that the blurring on both sides of the focus is the same. None of these assumptions is correct, but the equations above do give a usable model for the depth of focus. In practice, the acceptable blur diameter B is usually determined empirically by examining a series of defocused images to decide the level of acceptability; the equations above are then fitted to the results. 6.9

Diffraction Effects of Apertures

Even if we assume that an infinitely small point source of light is possible, no lens system can form a true point image, even though the lens be perfectly made and absolutely free of aberrations. This results from the fact that light does not really travel in straight-line rays, but behaves as a wave motion, bending around corners and obstructions to a small but finite degree. According to Huygen’s principle of light-wave propagation, each point on a wave front may be considered as a source of spherical wavelets; these wavelets reinforce or interfere with each other to form the new wave front. When the original wave front is infinite in extent, the new wave front is simply the envelope of the wavelets in the direction of propagation. At the other extreme, when the wave front is limited by an aperture to a very small size (say, to the order of a half wavelength), the new wave front becomes spherical about the aperture. Figure 6.13 shows a plane wavefront incident on a slit AC, which is in front of a perfect lens. The lens is focused on a screen, EF. We wish to determine the nature of the illumination on the screen. Since the lens of Fig. 6.13 is assumed perfect, the optical path lengths AE, BE, and CE are all equal and the waves will arrive in phase at E, reinforcing each other to produce a bright area. For Huygen’s wavelets

Figure 6.13

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Chapter Six

starting from the plane wave front in a direction indicated by angle , the paths are different; path AF differs from path CF by the distance CD. If CD is an integral number of wavelengths, the wavelets from A and C will reinforce at point F. If CD is an odd number of half wavelengths, a cancellation will occur. The illumination at F will be the summation of the contributions from each incremental segment of the slit, taking the phase relationships into account. It can be readily demonstrated that when CD is an integral number of wavelengths, the illumination at F is zero, as follows: if CD is one wavelength, then BG is one-half wavelength and the wavelets from A and B cancel. Similarly, the wavelets from the points just below A and B cancel and so on down the width of the slit. If CD is N wavelengths, we divide the slit into 2N parts (instead of two parts) and apply the same reasoning. Thus, there is a dark zone at F when ±N sin    w where N  any integer  the wavelength of the light w  the width of the slit Thus, the illumination in the plane EF is a series of light and dark bands. The central bright band is the most intense, and the bands on either side are successively less intense. One can realize that the intensity should diminish by considering the situation when CD is 1.5 , 2.5 , etc. When CD is 1.5 , the wavelets from two-thirds of the slit can be shown (as in the preceding paragraph) to interfere and cancel out, leaving the wavelets from one-third of the aperture; when CD is 2.5 , only one-fifth of the slit is uncanceled. Since the “uncanceled” wavelets are neither exactly in nor exactly out of phase, the illumination at the corresponding points on the screen will be less than onethird or one-fifth of that in the central band. For a more rigorous mathematical development of the subject, the reader is referred to the references following this chapter. The mathematical approach is one of integration over the aperture, combined with a suitable technique for the addition of the wavelets which are neither exactly in nor exactly out of phase. This approach can be applied to rectangular and circular apertures as well as to slits. For a rectangular aperture, the illumination on the screen is given by sin2 m1 sin2 m2  I  I0  m12 m22 wi sin i mi  

i  1,2

(6.16) (6.17)

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159

In these expressions is the wavelength, w the width of the exit aperture,  the angle subtended by the point on the screen, m1 and m2 correspond to the two principal dimensions, w1 and w2, of the rectangular aperture and I0 is the illumination at the center of the pattern. When the aperture is circular, the illumination is given by I  I0

冤

1 1  2

2J1(m)  I0  m

冤

m 2 1    2 3

冢 冣

冢

m2  222!

2

冣

1   4

冢

m3  2 33!

冥

2

冣

1   5

冢

m4  244!

2

冣

冥

2

 ...

2

(6.18)

where m is given by Eq. 6.17 with the obvious substitution of the diameter of the circular exit aperture for the width, w, and J1( ) is the firstorder Bessel function. The illumination pattern consists of a bright central spot of light surrounded by concentric rings of rapidly decreasing intensity. The bright central spot of this pattern is called the Airy disk. We can convert from angle  to Z, the radial distance from the center of the pattern, by reference to Fig. 6.14. If the optical system is reasonably aberration-free, then w l′   2 sin U′ and to a close approximation, when  is small l′ w Z     n′ 2n′ sin U′

(6.19)

The table of Fig. 6.15 lists the characteristics of the diffraction patterns for circular and slit apertures. The table is derived from Eqs. 6.16 and 6.18, but the data is given in terms of Z and sin U′ rather than  and w. Note that n′ sin U′ is the numerical aperture NA of the optical system. Notice that 84 percent of the energy in the pattern is contained in the central spot, and that the illumination in the central spot is almost 60 times that in the first bright ring. Ordinarily the central spot and

Figure 6.14

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Chapter Six

Figure 6.15 Tabulation of the size of and distribution of energy in the diffraction pattern

at the focus of a perfect lens.

the first two bright rings dominate the appearance of the pattern, the other rings being too faint to notice. The illumination in a diffraction pattern is plotted in Fig. 6.16. One should bear in mind the fact that these energy distributions apply to perfect, aberration-free systems with circular or slit apertures which are uniformly transmitting and which are illuminated by wave fronts of uniform amplitude. The presence of aberrations will, of course, modify the distribution as will any nonuniformity of transmission or wave-front amplitude (see, for example, Sec. 6.11). 6.10

Resolution of Optical Systems

The diffraction pattern resulting from the finite aperture of an optical system establishes a limit to the performance which we can expect from even the best optical device. Consider an optical system which images two equally bright point sources of light. Each point is imaged as an Airy disk with the encircling rings, and if the points are close, the diffraction patterns will overlap. When the separation is such that it is just possible to determine that there are two points and not one, the points are said to be resolved. Figure 6.17 indicates the summation of the two diffraction patterns for various amounts of separation. When the image points are closer than 0.5 /NA (NA is the numerical aperture of the system and equals n′ sin U′), the central maxima of both patterns blend into one and the combined patterns may appear to be due to a single source. At a separation of 0.5 /NA the duplicity of the image points is detectable, although there is no minimum between the maxima from the two patterns. This is Sparrow’s criterion for resolution. When the image separation reaches 0.61 /NA, the maximum

Stops and Apertures

161

Figure 6.16 The distribution of illumination in the Airy

disk. The appearance of the Airy disk is shown in the upper right.

of one pattern coincides with the first dark ring of the other and there is a clear indication of two separate maxima in the combined pattern. This is Lord Rayleigh’s criterion for resolution and is the most widely used value for the limiting resolution of an optical system.* From the tabulation of Fig. 6.15, we find that the distance from the center of the Airy disk to the first dark ring is given by 0.61 0.61 Z      1.22 (f/#) NA n′ sin U′

(6.20)

This is the separation of two image points corresponding to the Rayleigh criterion for resolution. This expression is widely used in determining the limiting resolution for microscopes and the like. For resolution at the image, the NA of the image cone is used; for resolution at the object, the NA of the object cone is used.

*The diffraction pattern of two point images will always differ somewhat from the diffraction pattern of a single point. It is thus possible to detect the presence of two points (as opposed to one) even in cases where the two points cannot be visually resolved or separated. This is the source of the occasional claims that a system “exceeds the theoretical limit of resolution.” In Chap. 11 it is shown that there is a true limit on the resolution of a sinusoidal line target; the limit on the spatial frequency is v0  2NA/  1/ (f/#).

162

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Figure 6.17 The dashed lines represent the diffraction

patterns of two point images at various separations. The solid line indicates the combined diffraction pattern. Case (b) is the Sparrow criterion for resolution. Case (c) is the Rayleigh criterion.

To evaluate the performance limits of telescopes and other systems working at long object distances, an expression for the angular separation of the object points is more useful. Rearranging Eq. 6.19 and substituting the limiting value of Z from Eq. 6.20, we get, in radian measure, 1.22    radians w

(6.21)

For ordinary visual instruments, may be taken as 0.55 m, and using 4.85 106 radians for 1 second of arc, we find that 5.5    seconds of arc (6.22) w when w is the aperture diameter expressed in inches. By a series of careful observations, the astronomer Dawes found that two stars of equal brightness could be visually resolved when their separation was 4.6/w seconds. Notice that if the Sparrow criterion is used instead of the Rayleigh criterion in Eq. 6.22, the limiting resolution angle is 4.5/w seconds, which is in close agreement with Dawes’ findings. It is worth emphasizing here that the angular resolution limit is a direct function of wavelength and an inverse function of the aperture of the system. Thus, the limiting resolution is improved by reducing

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163

the wavelength or by increasing the aperture. Note that focal length or working distance do not directly affect the angular resolution. The linear resolution is governed by the wavelength and the numerical aperture (NA or f-number), and not by the aperture diameter. In an instrument such as a spectroscope, where it is desired to separate one wavelength from another, the measure of resolution is the smallest wavelength difference, d , which can be resolved. This is usually expressed as /d ; thus, a resolution of 10,000 would indicate that the smallest detectable difference in wavelength was 1/10,000 of the wavelength upon which the instrument was set. For a prism spectroscope, the prism is frequently the limiting aperture, and it can be shown that when the prism is used at minimum deviation, the resolution is given by dn  B  d d

(6.23)

where B is the length of the base of the prism and dn/d is the dispersion of the prism material. A diffraction grating consists of a series of precisely ruled lines on a clear (or reflecting) base. Light can pass directly through a grating, but it is also diffracted. As with the slit aperture discussed above, at certain angles the diffracted wavelets reinforce, and maxima are produced when m sin    ±sin I S

(6.24)

where is the wavelength, I is the angle of incidence, S is the spacing of the grating lines, m is an integer, called the order of the maxima, and the positive sign is used for a transmission grating, the negative for a reflecting. (Note that a sinusoidal grating has only a first order.) Since  depends on the wavelength , such a device can be used to separate the diffracted light into its component wavelengths. When used as indicated in Fig. 6.18, the resolution of a grating is given by   mN d

(6.25)

where m is the order and N is the total number of lines in the grating (assuming the size of the grating to be the limiting aperture of the system). 6.11 Diffraction of a Gaussian (Laser) Beam The illumination distribution in the image of a point as described in Secs. 6.9 and 6.10 was based on the assumptions that the optical system was perfect and that both the transmission and the wave-front

164

Chapter Six

Figure 6.18 (Upper) Prism spectrometer. (Lower) Grating

spectrometer.

amplitude were uniform over the aperture. Any change in the intensity distribution in the beam will change the diffraction pattern from that described above. Obviously, a similar change in the transmission of the aperture will produce the same effects. A “gaussian beam” is one whose intensity cross section follows the equation of a gaussian, y  ex2. Laser output beams closely approximate gaussian beams. From mathematics we know that exponential functions, such as the gaussian are extremely resistant to transformations (consider, for example, the integral or differential of ex). Similarly, a gaussian beam tends to remain a gaussian beam, as long as it is “handled” by reasonably aberration-free optics, and the diffraction image of a point also has a gaussian distribution of illumination. The distribution of intensity in a gaussian beam is illustrated in Fig. 6.19 and can be described by Eq. 6.26. I (r)  Io e2r

2/w2

(6.26)

where I (r)  the beam intensity at a distance r from the beam axis I0  the intensity on axis r  the radial distance e  2.718.… w  the radial distance at which the intensity falls to I0 /e2, i.e., to 13.5 percent of its central value. This is usually referred to as the beam width, although it is a semidiameter. It encompasses 86.5 percent of the beam power.

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165

Figure 6.19 Gaussian beam intensity profile.

Beam power

By integration of Eq. 6.26 we find the total power in the beam to be given by Ptot  1/2 I 0w2

(6.27)

The power passed through a centered circular aperture of radius a is given by P (a)  Ptot(1  e2a

2/w2

)

(6.28)

The power passed by a centered slit of width 2s is given by

冕

s 兹苶 2 P (s)  Ptot erf  w

冢

冣

(6.29)

u

where erf (u)  0 et2 dt  the error function, which is tabulated in mathematical handbooks. Diffraction spreading of a gaussian beam

A gaussian beam has a narrowest width at some point, which is called the “waist.” This point may be near where the beam is focused or near where it emerges from the laser. As the beam progresses, it spreads out according to the following equation: z wz2  w02 1  2 w0

冤 冢

冣冥 2

(6.30)

where wz  the semidiameter of the beam (i.e., to the 1/e2 points) at a longitudinal distance z from the beam waist. w0  the semidiameter of the beam (to the 1/e2 points) at the beam waist.  the wavelength

166

Chapter Six

z  the distance along the beam axis from the waist to the plane of wz At large distances it is convenient to know the angular beam spread. Dividing both sides of Eq. 6.30 by z2, then, as z approaches infinity, we get 4 1.27 2  wz or      (6.31)        z w  (2w0) diameter 2  (2w0) 0 z→

where  is the angular beam spread in radians between the 1/e2 points. For many applications, the gaussian diffraction blur at the image plane can be found by simply multiplying  from Eq. 6.31 by the image conjugate distance (s′ from Chap. 2). Beam truncation

The effect of beam truncation, i.e., stopping down or cutting off the outer regions of the beam, is discussed by Campbell and DeShazer. They show that if the diameter of the beam is not reduced below 2(2w), where w is the beam semidiameter at the 1/e2 points, then the beam intensity distribution remains within a few percent of a true gaussian distribution. If the clear aperture is reduced below this value, it will introduce structure (i.e., rings) into the irradiance patterns, and the pattern gradually approaches Eq. 6.18 as the aperture is reduced. A lens aperture large enough to pass a beam with a diameter of 4w is obviously very inefficient from a radiation transfer standpoint. For this reason, most systems truncate the beam, very often to the 1/e2 diameter, and the diffraction pattern is altered accordingly. If the beam is truncated down to 61 percent of the 1/e2 diameter, it is difficult to see the difference from a uniform beam. Size and location of a new waist formed by a perfect optical system

When a gaussian beam passes through an optical system, a new waist is formed. Its size and location are determined by diffraction (and not by the paraxial equations of Chap. 2). The waist and focus are at different locations; in a weakly convergent beam, the separation may be large. The following equations allow calculation of the new waist size and location: xf 2 x′   w12 2 x2  

冢

冣

(6.32)

Stops and Apertures

f 2w12 x′  w12  w22   2 2 w 1 x x2  

冢

冣

冢 冣

167

(6.33)

where w1  the radius (to the 1/e2 points) of the original waist w2  the radius of the new waist formed by the optical system f  the focal length of the lens x  the distance from the first focal point of the lens to the plane of w1 x′  the distance from the second focal point of the lens to the plane of w2 Note that x and x′ are usually negative and positive, respectively. Note also the similarity to the newtonian paraxial equation (Eq. 2.3). Two points regarding the above are well worth emphasizing. First, laser researchers speak in terms of a “beam waist.” Note that in the equations above and in common usage it is described as a radial dimension, not a diameter; the diameter of the waist is 2w. Second, the waist and the focus are not the same thing, as a comparison of Eqs. 6.32 and 2.3 will indicate. In most circumstances the difference is trivial and gaussian beams may be handled by the usual paraxial equations. But when the beam convergence is small (i.e., with an f-number of a hundred or so), it is possible to distinguish both a focus and a separate beam waist. For example, if we project a 1-in laser beam (through a focusable beam expander) on a screen about 50 ft away, we can focus the beam to get the smallest possible spot on the screen. The focus is now at the screen. However, there is a location a few feet short of the screen at which a smaller beam diameter exists. This is the beam waist; it can be demonstrated by moving the screen (or a sheet of paper) toward the laser and observing the reduction of the spot size. Note that with the screen now at this beam waist position, the beam expander can be refocused to get a still smaller spot on the screen. Then there will be a new waist still closer to the laser, etc., etc., etc. Note well that the focus is the smallest spot which can be produced on a surface at a given, fixed distance. The waist is the smallest diameter in the beam (see Gaskill, p. 435). Note also that all the phenomena described in this section result from the gaussian distribution of beam intensity and not from the fact that the source may be a laser. The same effects could be produced by a radially graded filter placed over the aperture of the system. (The temporal and spatial coherence of a laser beam are, of course, what make it practical to demonstrate these effects.)

168

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OBJECT

FOURIER PLANE

LENS A

LENS B

IMAGE

COLLIMATED/ COHERENT ILLUMINATION

ƒ

ƒ

ƒ

ƒ

Figure 6.20

6.12 The Fourier Transform Lens and Spatial Filtering In Fig. 6.20 we have a transparent object located at the first focal point of lens A. As indicated by the dashed rays in the figure, lens A images the object at infinity so that the rays originating at the axial point of the object are collimated. These rays are brought to a focus at the second focal plane of lens B, where the image of the object is located. Now let us realize that Fourier theory allows us to consider the object as comprised of a collection of sinusoidal gratings of different frequencies, amplitudes, phases, and orientations. If our object is a simple linear grating with but a single spatial frequency, it will deviate the light through an angle  according to Eq. 6.24, except that a sinusoidal grating has but a single diffraction order, the first. Now, if the object is illuminated by collimated/coherent light, that diffracted light will be focused as two points in the second focal plane of lens A (which is indicated as the Fourier plane, midway between the lenses in Fig. 6.20). The points will be laterally displaced by   f tan  from the nominal focus. Thus, if an annular zone in the Fourier plane is obstructed, all the spatial information of the frequency corresponding to the radius of the obstruction will be removed (filtered) from the final image. Thus it can be seen that the Fourier plane constitutes a sort of map of the spatial frequency content of the object and that this content can be analyzed or modified in this plane. Bibliography Note: Titles preceded by an asterisk are out of print. Campbell, J., and L. DeShazer, J. Opt. Soc. Am., vol. 59, 1969, pp. 1427–1429. Gaskill, J., Linear Systems, Fourier Transforms, and Optics, New York, Wiley, 1978.

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169

Goodman, J., Introduction to Fourier Optics, New York, McGraw-Hill, 1968. *Hardy, A., and F. Perrin, The Principles of Optics, New York, McGraw-Hill, 1932. *Jacobs, D., Fundamentals of Optical Engineering, New York, McGraw-Hill, 1943. Jenkins, F., and H. White, Fundamentals of Optics, New York, McGraw-Hill, 1976. Kogelnick, H., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 7, New York, Academic, 1979. Kogelnick, H., and T. Li, Applied Optics, 1966, pp. 1550–1567. Pompea, S. M., and R. P. Breault, “Black Surfaces for Optical Systems,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 37. Silfvast, W. T., “Lasers,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 11. Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Office of Naval Research, 1985. Stoltzman, D., in Shannon and Wyant (eds.), Applied Optics and Optical Design, vol. 9, New York, Academic, 1983. *Strong, J., Concepts of Classical Optics, New York, Freeman, 1958. Walther, A., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965. Exercises 1 Find the positions and diameters of the entrance and exit pupils of a 100mm focal length lens with a diaphragm 20 mm to the right of the lens, if the lens diameter is 15 mm and the diaphragm diameter is 10 mm. ANSWER:

Entrance pupil is 25 mm to the right and 12.5 mm in diameter. Exit pupil is 20 mm to the right and 10 mm in diameter. 2 What is the relative aperture (f-number) of the lens of exercise #1 with light incident (a) from the left, and (b) from the right? ANSWER:

(a) f/8 (b) f/10

3 A telescope is composed of an objective lens, f  10 in, diameter  1 in and an eyelens, f  1 in, dia.  1 2 in, which are 11 in apart. (a) Locate the entrance and exit pupils and find their diameters. (b) Determine the object and image fields of view in radians. Assume object and image to be at infinity. ANSWER:

(a) Entrance pupil is at the objective, diameter 1 in. Exit pupil is 1.1 in to the right of the eyelens and is 0.1 in diameter. (b) For zero vignetting,

170

Chapter Six

object field is ±0.01818 and image field is ±0.1818. For complete vignetting, object field is ±0.02727 and image field is ±0.2727. 4 A 4-in focal length f/4 lens is used to project an image at a magnification of four times (m  4). What is the numerical aperture in object space and in image space? ANSWER:

NA  0.1; NA  0.025

5 An optical system composed of two thin elements forms an image of an object located at infinity. The front lens has a 16-in focal length, the rear lens an 8-in focal length, and the spacing between the two is 8 in. If the exit pupil is located at the rear lens and there is no vignetting, what is the illumination at an image point 3 in from the axis relative to the illumination on the axis? ANSWER:

41 percent

6 A 6-in diameter f/5 paraboloid mirror is part of an infrared tracker which can tolerate a blur (due to defocusing) of 0.1 milliradians. (a) What tolerance must be maintained on the position of the reticle with respect to the focal point? (b) What is the tolerance if the system speed is f/2? ANSWER:

(a) ±0.015 in (b) ±0.0024 in

7 If the hyperfocal distance of a 10-in focal length, f/10 lens is 100 in, (a) what is the diameter of the acceptable blur spot, and (b) what is the closest distance at which an object is “acceptably” in focus? (c) Show that the answer to (b) is always one-half the hyperfocal distance. ANSWER:

(a) 0.111 in (b) 50 in

8 Compare the image illumination produced by an f/8 lens at a point 45° from the axis with that from an f/16 lens 30° off axis. ANSWER:

The f/16 is 56 percent of the f/8

9 Plot the illumination (in the manner of Fig. 6.16) in the diffraction pattern at the focus of a lens with a square aperture, (a) along a line through the axis at 90° to a side of the aperture, and (b) along a line at 45° (the diagonal) to the sides of the aperture. 10 An optical system is required to image a distant point source as a spot of 0.01 mm in diameter. Assuming that all the useful energy in the image spot will be within the first dark ring, what relative aperture (f-number) must the optical system have? Assume a wavelength of 0.00055 mm. ANSWER:

f/7.5

11 A pinhole camera has no lens but uses a very small hole some distance from the film to form its image. If we assume that light travels in straight

Stops and Apertures

171

lines, then the image of a distant point source will be a blur whose diameter is the same size as the pinhole. However, diffraction will spread the light into an Airy disk. Thus, the larger the hole, the larger the geometrical blur but the smaller the diffraction pattern. Assume that the sharpest picture will be produced when the geometrical blur is the same size as the central bright spot of the Airy disk. What size hole should be used when the film is 10 cm from the hole? (Hint: Equate the hole diameter to the diameter of the first dark ring of the Airy disk given by Eq. 6.20.) ANSWER:

0.037 cm for  0.55 m (diameter 

兹2.44 苶f苶 )

12 What is the resolution limit (at the object) for a microscopic objective whose acceptance cone has a numerical aperture of (a) 0.25, (b) 0.8, (c) 1.2? ANSWER:

(a) 0.0013 mm, (b) 0.00042 nn, (c) 0.00028 mm

13 What diameter must a telescope objective have if the telescope is to resolve 11 seconds of arc? If the eye can resolve 1 minute of arc, what is the minimum power of the telescope? ANSWER:

0.5 in; 5.5 

14 Compare the resolution of a prism and a grating. The prism has a 1-in base and its glass has a dispersion of 0.1 per micrometer. The grating is 1-in wide and is ruled with 15,000 lines per inch. ANSWER:

Prism resolution—2540; grating resolution—15,000 1st order, 30,000 2d order, etc.

Chapter

7 Optical Materials and Interference Coatings

7.1 Reflection, Absorption, Dispersion To be useful as an optical material, a substance must meet certain basic requirements. It should be able to accept a smooth polish, be mechanically and chemically stable, have a homogeneous index of refraction, be free of undesirable artifacts, and of course transmit (or reflect) radiant energy in the wavelength region in which it is to be used. The two characteristics of an optical material which are of primary interest to the optical engineer are its transmission and its index of refraction, both of which vary with wavelength. The transmission of an optical element must be considered as two separate effects. At the boundary surface between two optical media, a fraction of the incident light is reflected. For light normally incident on the boundary the fraction is given by (n′  n)2 R  2 (n′  n)

(7.1)

where n and n′ are the indices of the two media (a more complete expression for Fresnel surface reflection is given in Sec. 7.9). Within the optical element, some of the radiation may be absorbed by the material. Assume that a 1-mm thickness of a filter material transmits 25 percent of the incident radiation at a given wavelength (excluding surface reflections). Then 2 mm will transmit 25 percent of 25 percent and 3 mm will transmit 0.25  0.25  0.25  1.56 percent.

173

174

Chapter Seven

Therefore, if t is the transmission of a unit thickness of material, the transmission through a thickness of x units will be given by T  tx

(7.2)

This relationship is often stated in the following form, where a is called the absorption coefficient and is equal to loge t. T  eax

(7.3)

Thus, it can be seen that the total transmission through an optical element is a sort of product of its surface transmissions and its internal transmission. For a plane parallel plate in air, the transmission of the first surface is given (from Eq. 7.1) as (n  1)2 4n T  1  R  1 2  2 (7.4) (n  1) (n  1) Now the light transmitted through the first surface is partially transmitted by the medium and goes on to the second surface, where it is partly reflected and partly transmitted. The reflected portion passes (back) through the medium and is partly reflected and partly transmitted by the first surface, and so on. The resulting transmission can be expressed as the infinite series T1.2  T1T2(K  K 3R1R2  K 5(R1R2)2  K7(R1R2)3  . . .)

(7.5)

T1T2 K   1  K 2R1R2 where T1 and T2 are the transmissions of the two surfaces, R2 and R1 are the reflectances of the surfaces, and K is the transmittance of the block of material between them. (This equation can also be used to determine the transmission of two or more elements, e.g., flat plates, by finding first T1,2 and R1,2, then using T1,2 and T3 together, and so on.) If we set T1  T2  4n/(n  1)2 from Eq. 7.4 into Eq. 7.5, and assume that K  1, we find that the transmission, including all internal reflections, of a completely nonabsorbing plate is given by 2n T   2 (n  1)

(7.6)

This is obviously the maximum possible transmission of an uncoated plate of index n. Similarly, the reflection is given by (n  1)2 R  1  T   (7.7) (n2  1)

Optical Materials and Interface Coatings

175

It should be emphasized that the transmission of a material, being wavelength-dependent, may not be treated as a simple number over any appreciable wavelength interval. For example, suppose that a filter is found to transmit 45 percent of the incident energy between 1 and 2 m. It cannot be assumed that the transmission of two such filters in series will be 0.45  0.45  20 percent unless they have a uniform spectral transmission (neutral density). To take an extreme example, if the filter transmits nothing from 1 to 1.5 m and 90 percent from 1.5 to 2 m, its “average” transmission will be 45 percent within the 1- to 2-m band. However, two such filters, when combined, will transmit zero from 1 to 1.5 m, and about 81 percent from 1.5 to 2 m, for an “average” transmission of about 40 percent, rather than the 20 percent which two neutral density filters would transmit. The photographic density of a filter is the log of its opacity (the reciprocal of transmittance), thus 1 D  log   log T T where D is the density and T is the transmittance of the material. Note that transmittance does not account for surface reflection losses; thus, density is directly proportional to thickness. To a fair approximation, the density of a “stack” of neutral density absorption filters is the sum of the individual densities. Equation 7.3 can be written to the base 10 if desired. This is done when the term “density” is used to describe the transmission of, for example, a photographic filter. The equation becomes T  10density so that a density of 1.0 means a transmission of 10 percent, a density of 2.0 means a transmission of 1 percent, etc. Note that densities can be added. A neutral absorbing filter with a density of 1.0 combined with a filter of density 2.0 will yield a density of 3.0 and a transmission of 0.1  0.01  0.001  103. Index dispersion

The index of refraction of an optical material varies with wavelength as indicated in Fig. 7.1 where a very long spectral range is shown. The dashed portions of the curve represent absorption bands. Notice that the index rises markedly at each absorption band, and then begins to drop with increasing wavelength. As the wavelength continues to increase, the slope of the curve levels out until the next absorption band is approached, where the slope increases again. For optical

176

Chapter Seven

Figure 7.1 Dispersion curve of

an optical material. The dashed lines indicate absorption bands. (Anomolous dispersion.)

materials we usually need concern ourselves with only one section of the curve, since most optical materials have an absorption band in the ultraviolet and another in the infrared and their useful spectral region lies between the two. Many investigators have attacked the problem of devising an equation to describe “the irrational variation of index” with wavelength. Such expressions are of value in interpolating between, and smoothing the data of, measured points on the dispersion curve, and also in the study of the secondary spectrum characteristics of optical systems. Several of these dispersion equations are listed below. c b Cauchy n ( )  a  2  4  . . . (7.8) d b Hartmann n ( )  a     (7.9) (c  ) (e  ) c b Conrady n ( )  a     (7.10) 3.5 d b Kettler-Drude n2 ( )  a  2  2  . . . c e Sellmeier Herzberger Old Schott

(7.11)

f 2 b 2 d 2 n2 ( )  a  2  2  2  . . . (7.12) c e g d e   (7.13) n ( )  a  b 2   2 2 (  0.035) (  0.035)2 f c d e (7.14) n2 ( )  a  b 2  2  4  6  8

The new Schott catalog uses the Sellmeier equation (Eq. 7.12). The constants (a, b, c, etc.) are, of course, derived for each individual material by substituting known index and wavelength values and solving the resulting simultaneous equations for the constants. The Cauchy equation obviously allows for only one absorption band at zero wavelength. The Hartmann formula is an empirical one but does allow absorption bands to be located at wavelengths c and e. The Herzberger expression is an approximation of the Kettler-Drude equation and is reliable through the visible to about 1 m in the near infrared. In his

Optical Materials and Interface Coatings

177

later work, Herzberger used 0.028 as the denominator constant. The Conrady equation is empirical and designed for optical glass in the visible region. All these equations suffer from the drawback that the index approaches infinity as an absorption wavelength is approached. Since little use is made of any material close to an absorption band, this is usually of small consequence. Equation 7.14 was used by Schott and other optical glass manufacturers as the dispersion equation for optical glass. It is accurate to about 3  106 between 0.4 and 0.7 m, and to about 5  106 between 0.36 and 1.0 m. The accuracy of Eq. 7.14 can be improved in the ultraviolet by adding a term in 4, and in the infrared by adding a term in 10. More recently, glass manufacturers have switched to Eq. 7.12, the Sellmeier equation, in order to improve the accuracy. The dispersion of a material is the rate of change of index with respect to wavelength, that is, dn/d . From Figs. 7.1 and 7.2, it can be seen that the dispersion is large at short wavelengths and becomes less at longer wavelengths. At still longer wavelengths, the dispersion increases again as the long-wavelength absorption band is approached. Notice in Fig. 7.2 that the glasses have almost identical slopes for wavelengths beyond 1 m. For materials which are used in the visible spectrum, the refractive characteristics are conventionally specified by giving two numbers, the index of refraction for the helium d line (0.5876 m) and the Abbe

INDEX OF REFRACTION

18

SAPPHIRE (AI2O3)

SF1 (717-295)

17 F4

SK8 (611-559) 16 F4 (617-366) BK7 (517-642) 15 BARIUM FLUORIDE (B0F2)

VISUAL RESP. .3

.5

1.0

1.5

2.0

2.5

WAVELENGTH IN MICRONS Figure 7.2 The dispersion curves for four optical glasses and two

crystals.

178

Chapter Seven

V-number, or reciprocal relative dispersion. The V-number, or V-value, is defined as nd  1 V  nF  nC

(7.15)

where nd, nF, and nC are the indices of refraction for the helium d line, the hydrogen F line (0.4861 m), and the hydrogen C line (0.6563 m), respectively. Note that n  nF  nC is a measure of the dispersion, and its ratio with nd  1 (which effectively indicates the basic refracting power of the material) gives the dispersion relative to the amount of bending that a light ray undergoes. For optical glass, these two numbers describe the glass type and are conventionally written (nd  1):V as a six-digit code. For example, a glass with an nd of 1.517 and a V of 64.5 would be identified as 517:645. For many purposes, the index and V-value are sufficient information about a material. For secondary spectrum work, however, it is necessary to know more, and the relative partial dispersion nd  nC PC   nF  nC

(7.16)

is frequently used for this purpose. PC is a measure of the rate of change of the slope of the index vs. wavelength curve (i.e., the curvature or second derivative). Note that a relative partial dispersion can be defined for any portion of the spectrum and that most glass catalogs list about a dozen partials. The index of refraction values conventionally given in catalogs, handbooks, etc., are those arrived at by measuring a sample piece in air, and are thus the index relative to the index of air at the wavelength, temperature, humidity, and pressure encountered in the measurement. Since the index is used in optical calculations as a relative number, this causes no difficulty if the index of air is assumed to be 1.0 (unless the optical system is to be used in a vacuum, in which case the catalog index must be adjusted for the index of air; see Sec. 1.2). 7.2

Optical Glass

Optical glass is almost the ideal material for use in the visual and near-infrared spectral regions. It is stable, readily fabricated, homogeneous, clear, and economically available in a fairly wide range of characteristics. Figure 7.3 gives some indication of the variety of the available optical glasses. Each point in the figure represents a glass whose nd is plotted against its V-value; note that the V-values are conventionally plotted in reverse, i.e., descending, order. Glasses are somewhat arbitrarily divided

Optical Materials and Interface Coatings

179

into two groups, the crown glasses and the flint glasses, crowns having a V-value of 55 or more if the index is below 1.60, and 50 or more for an index above 1.60; the flint glasses are characterized by V-values less than these limits. The “glass line” in Fig. 7.3 is the locus of the ordinary optical glasses made by adding lead oxide to crown glass. These glasses are relatively cheap, quite stable, and readily available. The addition of lead oxide to crown glass causes its index to rise, and its V-value to decrease, along the glass line. Immediately above the glass line are the barium crowns and flints; these are produced by the addition of barium oxide to the glass mix. In Fig. 7.3 these are identified by the symbol Ba for barium. This has the effect of raising the index without markedly lowering the V-value. The rare earth glasses are a completely different family of glasses based on the rare earths instead of silicon dioxide (which is the major constituent of the other glasses). These are identified by the symbol La in Fig. 7.3, signifying the presence of lanthanum. The table of Fig. 7.4 lists the characteristics of the most common optical glass types. Each glass type in the table is available from the major glass manufacturers, so that all types listed are readily obtainable. The index data given are taken from the Schott catalog; the equivalent glasses from other suppliers may have slightly different nominal characteristics. Formerly, optical glass was made by heating the ingredients in a large clay pot, or crucible, stirring the molten mass for uniformity, and carefully cooling the melt. The hardened glass was broken into chunks which were then sorted to select pieces of good quality. Currently the molten glass is more likely to be poured into a large slab mold; this gives better control over the size of the pieces of glass available. Many barium glasses and all the rare earth glasses are processed in platinum crucibles, since the highly corrosive molten glass tends to attack the walls of a clay pot and the dissolved pot materials affect the glass characteristics. In extremely large volume production, a continuous process is used, with the raw materials going in one end of the furnace and emerging as extruded strip or rod glass at the other end. Raw glass is frequently pressed into blanks, which are roughly the size and shape of the finished element. The final stage before the glass is ready for use is annealing. This is a slow cooling process, which may take several days or weeks, and which relieves strains in the glass, assures homogeneity of index, and brings the index up to the catalog value. The characteristics of optical glass vary somewhat from melt to melt (because of variations in composition and processing) and also due to variations in annealing procedures. Ordinarily the lower index glasses (to n  1.55), are supplied to a tolerance of ±0.001 on the catalog value of nd, the higher index glasses may vary ±0.0015 from the nom-

180

(Abbe V-value). The glass types are indicated by the letters in each area. The “glass line” is made up of the glasses of types K, KF, LLF, LF, and SF which are strung along the bottom of the veil. (Note that K stands for kron, German for “crown,” S stands for schwer, or “heavy or dense.”) (Courtesy of Schott Glass Technologies, Inc., Duryea, Pa.)

Figure 7.3 The “glass veil.” Index (nd) plotted against the reciprocal relative dispersion

181

indicating the resistance of the glass to staining or hazing due to environmental attack; the higher the number, the lower the resistance;  is the thermal expansion coefficient, and Tg is the transformation temperature. D is the density, HK is the Knoop hardness, and i is the internal transmittance at 0.4 m for a thickness of 25 mm.

Figure 7.4 Characteristics of a selection of optical glasses. CR, FR, SR, and AR are codes

182

Figure 7.4

Continued

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inal index. Similarly the V-value will vary from the catalog value. Typical tolerances on V-value are ±0.3 for V-values below 46; ±0.4 from 46 to 58; ±0.5 for V-values above 58. Most glass manufacturers will select glass to closer tolerances at an increased price. Optical glass may be obtained in hundreds of different types; complete information is best obtained from the manufacturer’s catalog. Figure 7.5 gives an indication of the spectral transmission of optical glasses. In general, most optical glasses transmit well from 0.4 to 2.0 m. The heavy flints tend to absorb more at the short wavelengths and transmit more at the long wavelengths. The rare earth glasses also absorb in the blue region. Since the transmission of a glass is affected greatly by minute impurities, the exact characteristics of any given glass may vary significantly from batch to batch, even when made by the same manufacturer. Most optical glasses turn brown (or black) when exposed to nuclear radiation because of increased absorption of the short (blue) wavelengths. To provide glasses which can be used in a radiation environment, the glass manufacturers have developed “protected” or “nonbrowning” glasses containing cerium. These glasses will tolerate radiation doses to the order of a million roentgens. Fused quartz glass, which is discussed in the next section, is almost pure SiO2 and is extremely resistant to radiation browning. Although not strictly “optical glass,” ordinary window glass and plate glass are frequently used when cost is an important factor. The index of window glass ranges from about 1.514 to about 1.52, depending on the manufacturer. Ordinary window glass is slightly greenish, due primarily to modest amounts of absorption in the red and blue wavelengths; the red absorption continues to about 1.5 m. Window glass is also available in “water white” quality, without the greenish tint. For elements with one or two plane surfaces and with modest precision requirements, window glass can often be used without further processing; the accuracy of the plane surfaces is surprisingly good. By special selection, plane parallels can be obtained which meet fairly rigorous requirements. The secret here is to avoid pieces cut from the edge of the large sheets in which this type of glass is made; the center sections are usually far more uniform in surface and thickness. Note that the surface of “float glass” is significantly less smooth by a factor of 3 or 4, although recent process improvements have brought the surfaces up to that of window and plate glass. 7.3 Special Glasses Several glasses are available which differ sufficiently from the standard optical glasses to deserve special mention.

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glass, all for a thickness of 25 mm.

Figure 7.5 Internal transmittance of several representative optical glasses plus window

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Low-expansion glasses. In applications where the elements of an opti-

cal system are subject to strong thermal shocks (as in projection condensers) or where extreme stability in the presence of temperature variations is necessary (such as astronomical telescope reflectors or laboratory instruments), it is desirable to use a material with a low thermal coefficient of expansion. A number of borosilicate glasses are made with expansion coefficients which are less than half that of ordinary glass. Corning’s Pyrex #7740 and #7760 have expansion coefficients between 30 and 40  107/°C. The index of refraction of these glasses is about 1.474 with a V-value of about 60, and their density is about 2.2. Unfortunately they are usually afflicted with veins and striations so that they are suitable only for applications such as condensing systems when used as refracting elements. They are widely used for test plates and for mirrors. Some of these materials are yellowish or brownish, but others are available in a clear white grade. Another low-expansion glass is fused quartz, which is also called fused silica glass. This material is essentially pure (more or less, depending on the grade and manufacturer) silicon dioxide (SiO2) and has an extremely low expansion coefficient of 5.5  107/°C. It was originally made by fusing powdered crystalline quartz. Fused quartz can be obtained in grades with homogeneity equal to that of optical glass. Fused glass is a completely different material than crystalline quartz. Its index is 1.46 versus 1.55; it is amorphous (glassy) without crystalline structure; and it is not birefringent, as is quartz. Fused quartz has excellent spectral transmission characteristics, extending further into both the ultraviolet and infrared than ordinary optical glass. For this reason it is frequently used in spectrophotometers, infrared equipment, and ultraviolet devices. The excellent thermal stability of fused quartz is responsible for its use where extremely precise reflecting surfaces are required. Large mirrors and test plates are frequently made from fused quartz for this reason. As previously mentioned, pure fused quartz is highly resistant to radiation browning. The index of refraction and transmission of fused quartz are given in Fig. 7.6. Note that the absorption bands indicated are not of the type indicated in Fig. 7.1, but are due to impurities and are thus subject to elimination, as indicated by the range of transmissions given. A new class of materials, which are partially crystallized glasses, is available for use as extremely thermally stable mirror substrates, since they can be fabricated with a zero thermal expansion coefficient. Owens-Illinois CER-VIT was the original material; Corning ULE and Schott ZERODUR have similar properties. These materials can be tailored to have a zero thermal expansion coefficient (plus or minus about 1  107) at a given temperature. The zero thermal expansion coeffi-

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Figure 7.6 Optical characteristics of fused quartz.

cient results from the mixture of crystals (with a negative coefficient) and amorphous glass with a positive coefficient. These materials tend to be brittle, yellow or brown, and to scatter light, so they are not suitable for refracting optics. Infrared transmitting glasses. A number of special “infrared” glasses are

available. Some of these are much like extremely dense flint glasses, with index values of 1.8 to 1.9 and transmitting to 4 or 5 m. The arsenic glasses transmit even further into the infrared. Arsenic-modified selenium glass transmits from 0.8 to 18 m, but will soften and flow at 70°C. It has the following index values: 2.578 at 1.014 m; 2.481 at 5 m; 2.476 at 10 m; 2.474 at 19 m. Arsenic trisulfide glass transmits from 0.6 to 13 m and is somewhat brittle and soft. Index values: 2.6365 at 0.6 m; 2.4262 at 2 m; 2.4073 at 5 m; 2.3645 at 12 m.

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Gradient index glass. As indicated in Chap. 1, if the index of refraction

is not uniform, light rays travel in curved paths rather than in straight lines. In visualizing this, it often helps to remember that the light rays curve toward the region of higher index. If the index varies in a controlled way, this property may be advantageously utilized. Glass can be doped by infusion with other materials, typically by the immersion of the glass into a bath of molten salts to effect an ion exchange which produces a changed index. A gradient also can be produced by fusing together layers of glasses with differing indexes. Several types of index gradient are useful in optical systems. A radial gradient has an index which varies with the radial distance from the optical axis. An axial gradient varies the index with the distance along the axis. A spherical gradient varies the index as a function of the radial distance from an axial point. An axial gradient at a spherical surface has an effect on the aberrations which is quite analogous to that of an aspheric surface. A radial gradient can produce lens power in a plano-plano element. For example, a plano element whose index varies as a function of the radial distance r according to n (r)  n0(1  Kr2) and has a length L will have a focal length given by 1 f   n0 兹苶 2K sin (L 兹苶 2K ) and a back focal length of 1 bf l   n0 兹苶 2K tan (L 兹苶 2K ) This effect is the basis of the GRIN rod lens and the SELFOC lens. 7.4 Crystalline Materials The valuable optical properties of certain natural crystals have been recognized for years, but in the past the usefulness of these materials was severely limited by the scarcity of pieces of the size and quality required for optical applications. However, many crystals are now available in synthetic form. They are grown under carefully controlled conditions to a size and clarity otherwise unavailable. The table of Fig. 7.7 lists the salient characteristics of a number of useful crystals. The transmission range is indicated in micrometers for a 2-mm-thick sample; the wavelengths given are the 10 percent transmission points. Indices are given for several wavelengths in the transmission band.

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Crystal quartz and calcite are infrequently used because of their birefringence, which limits their usefulness almost entirely to polarizing prisms and the like. Sapphire is extremely hard and must be processed with diamond powder. It is used for windows, interference filter substrates, and occasionally for lens elements. It is slightly birefringent, which limits the angular field over which it can be used. The halogen salts have good transmission and refraction characteristics, but their physical properties often leave much to be desired, since they tend to be soft, fragile, and occasionally hygroscopic. Germanium and especially silicon are widely used for refracting elements in infrared devices. They are much like glass in their physical characteristics, and can be processed with ordinary glass-working techniques. Both are metallic in appearance, being completely opaque in the visible. Their extremely high index of refraction is a joy to the lens designer since the weak curvatures which result from the high index tend to produce designs of a quality which cannot be duplicated in comparable glass systems. Special low-reflection coatings are necessary since the surface reflection (per Eq. 7.1 et seq.) is very high, for example, 36 percent per uncoated germanium surface. Zinc sulfide, zinc selenide, and AMTIR are also widely used in infrared systems. Worthy of special mention is calcium fluoride, or fluorite. This material has excellent transmission characteristics in both ultraviolet and infrared, which make it valuable for instrumentation purposes. In addition, its partial dispersion characteristics are such that it can be combined with optical glass to form a lens system which is free of secondary spectrum. Its physical properties are not outstanding since it is soft, fragile, resists weathering poorly, and has a crystal structure which sometimes makes polishing difficult. In exposed applications, the fluorite element can sometimes be sandwiched between glass elements to protect its surfaces. The table of Fig. 7.8 lists selected index and transmission values for fluorite. Natural fluorite has been used in microscope objectives for many, many years. The FK glasses, especially FK51, FK52, and FK54, share many of fluorite’s characteristics and are very useful in correcting secondary spectrum. 7.5 Plastic Optical Materials Plastics are rarely used for high precision optical elements. A great deal of effort was made to develop plastics for optical systems during the Second World War, and a few systems incorporating plastics were produced. Since then, the technology of fabrication of plastic optics has advanced significantly, and today, in addition to novelty items such as toys and magnifying glasses, plastic lenses can be found in a multitude of optical applications, including inexpensive, disposable camera lens-

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Figure 7.7 Characteristics of optical crystals.

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Figure 7.8 Index and transmission of calcium fluoride (CaF2) for various

wavelengths.

es, many zoom lenses, projection TV lenses, and even some highquality camera lenses. The low cost of mass-produced plastic optics is one important factor in this popularity; another is the ease of production of aspheric surfaces. Once the aspheric mold has been fabricated, an aspheric surface is as easy to make as is a spherical surface (in marked contrast to glass optics). The rule of thumb that the introduction of an aspheric surface allows the elimination of an element from the system attests to the value of optical plastic materials. This aspheric capability largely offsets the unfortunate fact that the number of suitable optical plastics is very small and that there are only relatively low index materials in that number. In considering a venture into the plastic optics arena, one is well advised to seek out a specialist in making plastic optics. Not only is the typical injection molder incapable of making good optics, but he or she also has no conception of what is required to do so. The successful fabricators have developed good, reliable sources of consistently highquality raw materials and material handling techniques, and they have molding machines which have been adapted to the special requirements of optical work. Temperature control is extremely critical, and a longer cycle time is necessary to achieve an optical level of precision. I encountered an extreme case a few years ago. I had designed a visual system for a client who insisted (against my advice) not only on patronizing an inexperienced (in optics) injection molder but also on

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using an unusual material. The result was a system which you literally could not see through. In addition to the general, smooth aspheric capability, plastics are widely used to make Fresnel lenses, where fine steps are necessary. The condenser system in overhead projectors and the field lenses in the viewfinders of single-lens reflex cameras are examples of plastic Fresnel lenses (see Sec. 9.6). Another currently popular application is in diffractive optics (discussed at greater length in Chaps. 9 and 13), where the diffractive surface is basically a Fresnel surface whose step height is on the order of a half wavelength. Another advantage in mass production is the ability to mold both the lens element and its mounting cell in one shot. The cells of an assembly can in fact be designed so that the lens assembly simply snaps together, and a drop of a suitable solvent can make the assembly permanent. The obvious advantages of plastic—that it is light and relatively shatterproof—are offset by a number of disadvantages. It is soft and scratches easily. Except by molding, it is difficult to fabricate. Styrene plastic is frequently hazy, scatters light, and is occasionally yellowish. Plastics tend to soften at 60 to 80°C. In some plastics the index is unstable and will change as much as 0.0005 over a period of time. Most plastics will absorb water and change dimensionally; almost all are subject to cold flow under pressure. The thermal expansion coefficient is almost 10 times that of glass, being 7 or 8  105/°C. The change of index with temperature for plastics is very large (about twenty times that of glass) and negative. Thus, maintaining focus over a range of temperature is a significant problem for plastic optics. Often they must be athermalized as well as achromatized. The density of plastics is low, usually to the order of 1.0 to 1.2. The characteristics of some of the most widely used optical plastics are summarized in Fig. 7.9. Another optical application for plastics is in replication. In this process a precisely made master mold is vacuum-coated with a release, or parting layer, plus any required high- or low-reflection coatings. (The nature of the release layer is usually considered proprietary, but very thin layers of silver, salt, silicone, or plastic have been publicly mentioned.) Next, a few drops of low-shrinkage epoxy are pressed out into a thin (ideally about 0.001 or 0.002 in thick) layer between the master and a closely matching substrate. The substrate may be Pyrex, ceramic, or very stable aluminum (for reflector optics), or glass (for refracting optics). When the epoxy has cured, the master is removed and a reasonably precise (negative) replica is left on the substrate. This process has several advantages. For example, any surface (including aspherics) for which a master can be made can be replicat-

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Figure 7.9 Properties of several optical plastics. (From Lytel and Altman.) Note that

index values may vary significantly from one manufacturer to another.

ed relatively inexpensively, since the master can be used over and over. Other advantages are that a mirror can be made an integral part of its mount, the bottom of a blind hole can have an optical polish and figure, and extremely thin and lightweight parts can be produced. In many cases these things are effectively impossible with standard optical fabrication techniques. The limitations to replicated parts are the inherent softness of the epoxy and the change in the surface figure from that of the mold. 7.6

Absorption Filters

Absorption filters are composed of materials which transmit light selectively; that is, they transmit certain wavelengths more than others. A small percentage of the incident light is reflected, but the major portion of the energy which is not transmitted through the filter is absorbed by the filter material. Obviously, every material discussed in the preceding sections of this chapter is, in the broadest sense, an absorption filter, and occasionally these materials are introduced into optical systems as filters. However, most filters are made by the addition of metallic salts

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to clear glass or by dyeing a thin gelatin film to produce a more selective absorption than is available in “natural” materials. The prime source of dyed gelatin filters is the Eastman Kodak Company, whose line of Wratten filters is widely used for applications where the versatility of dyed gelatin is required and the environmental requirements are not too severe. Gelatin filters are usually mounted between glass to protect the soft gelatin from damage. The number of coloring materials which are suitable for use in optical filter glass is limited, and the types of filter glass available are thus not as extensive as one might desire. In the visible region, there are several main types. The red, orange, and yellow glasses all transmit the red and near-infrared and have a fairly sharp cutoff, as indicated in Fig. 7.10. The position of this cutoff determines the apparent color of the filter. Green filters tend to absorb both the red and blue portions of the spectrum. Their transmission curves often resemble the spectral sensitivity curve of the eye. Blue optical glass filters can be a disappointment, since they occasionally transmit not only blue light, but some green, yellow, orange, and frequently a sizable amount of red light as well. The purple filters transmit both the red and blue ends of the spectrum, with fair suppression of the yellow and green spectral regions. Filter glass is manufactured by most optical glass companies

Figure 7.10 Spectral transmission curves for several optical glass filters.

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as well as a number of establishments which make commercial colored glass (as opposed to “optical” glass, which is more carefully controlled). The transmission characteristics of glass filters vary from melt to melt for any given type. If a filter application requires that the transmission be accurately controlled, it is frequently necessary to adjust the finished thickness of the filter to compensate for these variations. The red filters are probably the most variable; since they are sensitive to heat, some red glasses cannot be re-pressed into blanks. Spectral transmission data for filters is usually given for a specific thickness and includes the losses due to Fresnel surface reflections. To determine the transmission for thicknesses other than the nominal value, the transmittance, that is, the “internal” transmission of the piece without the reflection losses, must be determined. In most cases, it is sufficient to divide the transmission by Eq. 7.4 to get the transmittance. Then Eq. 7.2 or 7.3 can be used to determine the transmittance of the new thickness. This transmittance times the T of Eq. 7.4 will then give the total transmission for the filter to a reasonable accuracy. This process is greatly simplified by the use of a log-log plot of the transmittance. The Schott catalog of filter glass makes use of this type of scale. A transparent overlay makes it possible to evaluate instantly the effect of a thickness change. A study of Fig. 7.11 will indicate the utility of this type of a transmittance plot; the same filter is shown in two thicknesses on a log-log scale in the upper figure and on a linear scale in the lower. Against the log-log scale, the thickness change is effected by a simple vertical displacement of the plot. The amount of the displacement is given by the thickness scale at the right. Notice how much more information this type of plot can give (and how much more is required to prepare one!). The data plotted in this form is transmittance; to determine the total transmission of the filter, the surface reflection losses must be taken into account, either by Eq. 7.4 or 7.5. Glass filters are also available to transmit either the ultraviolet or infrared regions of the spectrum without transmitting the visible. Typical transmission plots for these filters are shown in Fig. 7.12. Heat-absorbing glasses are designed to transmit visible light and absorb infrared energy. These are frequently used in projectors to protect the film or LCD from the heat of the projection lamp. Since they absorb large quantities of radiant energy, they become hot themselves and must be carefully mounted and cooled to avoid breakage from thermal expansion. From the spectral transmission characteristics given in Fig. 7.12, it is apparent that the phosphate heat-absorbing glass is more efficient than the Aklo; the phosphate glass is subject to large bubbles and inclusions which do not, however, prevent its use in

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Figure 7.11 Spectral transmittance of Schott KG2 heat-absorbing filter glass. The upper

graph is plotted on a log-log scale. Note that the vertical spacing between the two plots is equal to the distance from 2 to 5 on the thickness scale at the right. The same data is plotted on a conventional linear scale in the lower figure for comparison.

most applications. See also the discussion of “hot” and “cold” mirrors in Sec. 7.10. 7.7 Diffusing Materials and Projection Screens A piece of white blotting paper is an example of a (reflecting) diffusing material. Light which strikes its surface is scattered in all directions; as a result, the paper appears to have almost the same brightness regardless of the angle at which it is illuminated or the angle from which it is viewed. A perfect, or lambertian, diffuser is one which has the same apparent brightness from any angle; thus the radiation emitted per unit area in the surface is given by I0 cos , where  is the angle

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Figure 7.12 Transmission characteristics of special-purpose glass filters. UV

transmitting: solid line, Corning 7-60; dashed, Corning 7-39. IR transmitting solid, Corning 7-56 (#2540); dashed, Corning 7-69; dotted, Schott UG-8. Heat absorbing: solid, Corning I-59 extra light Aklo; dashed, Pittsburgh Plate Glass #2043 Phosphate—2 mm; dotted, Corning I-56 dark shade Aklo.

to the surface normal and I0 is the intensity of an element of area in a direction perpendicular to the surface. There are a number of quite good reflecting diffusers with relatively high efficiencies. Matte white paper is a very convenient one and reflects 70 to 80 percent of the incident visible light. Magnesium oxide and magnesium carbonate are frequently used in photometric work since their efficiencies are high, to the order of 97 or 98 percent. The brightness (luminance) of a perfectly diffuse reflector is proportional to the illumination falling on it and to its reflectivity. If the illumination is measured in footcandles, multiplication by the reflectivity yields the brightness in foot-lamberts. The brightness in lamberts is given by the illumination in lumens per cm2 times the reflectivity, and if this product is divided by , the result is the brightness in candles per cm2, or in lumens per steradian per cm2. (See Chap. 8 for more material on photometric considerations.) As indicated above, a perfectly diffuse surface appears to have the same brightness regardless of the angle at which it is viewed. A projec-

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tion screen which is not perfectly diffuse can have a brightness ranging from zero to that of the projector light source. For example, consider a perfect mirror screen in the shape of an ellipsoid, with the viewer’s eye placed at one focus and the projector at the other. All of the light will be reflected to the eye; none will be scattered. From this eye position the screen will have the same brightness as if one looked directly into the projection lens; when viewed from any other location, the screen will appear completely dark. The gain of a projection screen is the ratio of its brightness to that of a perfectly diffuse (or lambertian) screen, which by definition has a gain of 1.0. A diffuse screen can be viewed from any direction, and its brightness, while low, is independent of the viewing angle. The higher the gain of a screen, the smaller the angle over which it has its rated gain. Beaded screens and facetted, lenticular screens are used to concentrate and distribute the light in a controlled manner. Aluminum paints are used to coat screens which must maintain polarization, and with a smooth curved surface can achieve gains as high as 4.0 in commercial products. Beaded screens can achieve a gain as high as 10, but only over an extremely restricted angle. Many projection screens are rated at a gain of about 2.0. Transmitting diffusers are used for such applications as rear projection screens and to produce even illumination. The most commonly used are opal glass and ground glass (Fig. 7.13). Opal glass contains a suspension of minute colloidal particles and diffuses by multiple scattering from these particles. The transmitted light is slightly yellowish

Figure 7.13 Polar intensity plots

of diffusing materials. (Left) For a “perfect diffuser, the intensity of a unit area of the surface varies with cos . (Right) The relative intensities of singleand double-ground glass and flashed opal glass.

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since the shorter wavelengths are scattered more than the longer. Opal glass is ordinarily used as flashed opal, which is a thin layer of opal glass fused to a supporting sheet of clear glass. The diffusion of flashed opal is quite good. When illuminated normally, the brightness at 45° from the normal is about 90 percent of what one would expect from a perfect diffuser. Its total transmission is quite low, about 35 or 40 percent. It should be noted that, since good diffusion means that the incident light is scattered into 2 steradians, the axial brightness of a rear-illuminated screen of good diffusion is very low when compared with a poor diffuser. Ground glass is produced by fine grinding (or etching) the surface of a glass plate to produce a large number of very small facets which refract the incident light more or less randomly. The total transmission of ground glass is about 75 percent. This transmission is quite strongly directional, and ground glass is far from a perfect diffuser. Its characteristics vary somewhat, depending on the coarseness of the surface. Typically, for a normally illuminated surface, the brightness at 10° from the normal is about 50 percent of the normal brightness; at 30°, the brightness is about 2.5 percent of the brightness at the normal. This characteristic is of course quite useful when partial diffusion is desired. By combining two sheets of ground glass (with the ground faces in contact), the transmission is lowered about 10 percent but the diffusion is improved; at 20° to the normal, the brightness is about 20 percent; at 30°, about 7 percent. With two sheets, the diffusion can be increased by spacing them apart, although this will destroy their utility as a projection screen. A sheet of tracing paper has diffusion characteristics quite similar to ground glass, and there are several commercially available plastic screen materials which are somewhat better diffusers than ground glass. The plastic surface also can be shaped to control the beam spread. A rear projection screen, when used in a lighted room, is illuminated from both sides. The room light reduces the contrast of the projected image. This situation is sometimes alleviated by introducing a sheet of gray glass (that is, a neutral filter) between the diffusing screen and the observer. When this is done, the light from the projector is reduced by a factor of T, the transmission of the gray glass, but the room light is reduced by T 2, since the room light must pass through the gray glass twice to go from the room to the diffuser and back to the observer’s eye. 7.8 Polarizing Materials Light behaves as a transverse wave in which the waves vibrate perpendicular to the direction of propagation. If the wave motion is considered as a vector sum of two such vibrations in perpendicular planes, then plane polarized light results when one of the two compo-

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nents is removed from a light beam. Plane polarized light can be produced by passing the radiation from an ordinary source through a polarizing prism, several types of which are available. These prisms depend on the birefringent characteristic of calcite (CaCO3), which has a different index of refraction for the two planes of polarization. Since light of one polarization is refracted more strongly than the other, it is possible to separate them either by total internal reflection (as in the Nicol and Glan-Thompson prisms) or by deviation in different directions (as in the Rochon and Wollaston prisms). Such prisms are large, heavy, and expensive. Sheet polarizers, which are made by aligning microscopic crystals in a suitable base, are thin, light, relatively inexpensive, useful over a wide field of view, and simple to fabricate into an almost unlimited range of sizes and shapes. Thus, despite the fact that they are not quite as efficient as a good prism polarizer and are not effective over as large a wavelength range, they have largely supplanted prisms for the great majority of applications where polarization is required. The Polaroid Corporation of Cambridge, Massachusetts, produces a number of types of sheet polarizers. For work in the visible region, several types are available, depending on whether optimum transmission or optimum extinction (through crossed polarizers) is desired. Special types are available for use at high temperatures and also for use in the near-infrared (0.7 to 2.2 m). Polaroid also produces circular (as opposed to plane) polarizers in sheet form. Since a plane polarizer will eliminate half the energy, it is obvious that the maximum transmission of a “perfect” polarizer in a beam of unpolarized light will be 50 percent. Practical values range from 25 to 40 percent for sheet Polaroid, depending on the type. If two polarizers are “crossed,” that is, oriented with their polarizing axes at 90°, the transmission will be zero if the polarization is complete. This can be achieved with Nicol prisms, but the sheet polarizers have a residual transmission ranging from 106 to 5  104, again dependent on the type. The transmission characteristics of sheet polarizers are wavelength-dependent as well. When two polarizers are placed in a beam of unpolarized light, the transmission of the pair depends on the relative orientation of their polarization axes. If  is the angle between the axes, then the transmission of the pair is given by: T  K 0 cos2   K90 sin2 

(7.17)

where K0 is the maximum transmission and K90 is the minimum. Typical value pairs for K0 and K90 are 42 percent and 1 or 2 percent; 32 percent and 0.005 percent; 22 percent and 0.0005 percent. Reflection from the surface of a glass plate may also be used to produce plane polarized light. When light is incident on a plane surface at

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Brewster’s angle, one plane of polarization is completely transmitted (if the glass is perfectly clean) and about 15 percent of the other is reflected. This occurs when the reflected and refracted rays are at 90° to each other; thus, Brewster’s angle is given by n′ I  arctan  n

(7.18)

The reflected beam is thus completely polarized and the transmitted beam partially so. The percentage of polarized light in the transmitted beam can be increased by using a stack of thin plates all tilted to Brewster’s angle. For an index of 1.52, Brewster’s angle is 56.7°. Note that Brewster’s angle is the angle at which the tangent term in Eq. 7.19 goes to zero. The subject of polarized light is treated at greater length in texts devoted to physical optics, to which the reader is referred. Two additional points are worth noting: one, interference filters (Sec. 7.9) are usually polarizing and are occasionally used as polarizers; and two, opal glass and other diffusers are excellent depolarizers, as are integrating spheres. 7.9 Dielectric Reflection and Interference Filters The portion of the light reflected (Fresnel reflection) from the surface of an ordinary dielectric material (such as glass) is given by 1 R  2

冤

tan2 (I  I′) sin2 (I  I′)    sin2 (I  I′) tan2 (I  I′)

冥

(7.19)

where I and I′ are the angles of incidence and refraction, respectively. The first term of Eq. 7.19 gives the reflection of the light which is polarized normal to the plane of incidence (s-polarized), and the second term the reflection for the other plane of polarization (p-polarized). As indicated in Sec. 7.1, at normal incidence Eq. 7.19 reduces to (n′  n)2 R  2 (n′  n)

(7.20)

The variation of reflection from an air-glass interface as a function of the angle of incidence (I) is shown in Fig. 7.14, where the solid line is R, the dashed line is the sine term, and the dotted line is the tangent term. Notice that the dotted line drops to zero reflectivity at Brewster’s angle (Eq. 7.18). The reflection from more than one surface can be treated as indicated by Eq. 7.5 when the separation between the surfaces is large compared to the wavelength of light. However, when the surface-to-surface

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Figure 7.14 The reflection from

a single air-glass interface (for an index of 1.523). Solid line is the reflection of unpolarized light. The fine dashed line is the reflection of p-polarized light, with the electric field vector parallel to the plane of incidence. The heavier dashed line is for the s-polarization. (Note that the “plane of polarization” was originally defined to be at right angles to what we now call the plane of polarization/vibration.)

separation is small, then interference between the light reflected from the various surfaces will occur and the reflectivity of the stack of surfaces will differ markedly from that given by Eq. 7.5. (At this point the reader may wish to refer to the discussion of interference effects contained in the first chapter.) Optical coatings are thin films of various substances, notably magnesium fluoride (MgF2, n  1.38), zinc sulfide (ZnS, n  2.3), silicon monoxide (SiO, n  1.86), tantalum pentoxide (Ta2O5, n  2.15), thorium fluoride (ThF4), lanthanum trifluoride (LaF3, n  1.57), cerium fluoride (CeF3, n  1.60), hafnium oxide (HfO2, n  2.05), neodmium fluoride (NdF3) and yttrium oxide (Y2O3, n  1.85), among others, which are deposited in layers on an optical surface for the purpose of controlling or modifying the reflection and transmission characteristics of the surface. Such films have an optical thickness (index times mechanical thickness) which is a fraction of a wavelength, usually onequarter or one-half wavelength. The deposition of thin films is carried out in a vacuum and is done by heating the material to be deposited to its evaporation temperature and allowing it to condense on the surface to be coated. The thickness of the film is determined by the rate of evaporation (or more precisely, condensation) and the length of time the process is allowed to continue. Since interference effects produce colors in the light reflected from thin films, just as in oil films on wet pavements, it is possible to judge the thickness of a film by the apparent color of light reflected from it. Simple coatings can be controlled visually by utilizing this effect, but coatings consisting of several layers are often monitored photoelectrically, using monochromatic light, so that the sinusoidal rise and fall of the reflectivity can be accurately assessed and the thickness of each layer controlled. By using two different wavelengths (often from lasers), this technique can achieve high

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precision. Another popular monitoring technique utilizes a quartz crystal of the type used to control radio broadcast frequencies. The oscillation frequency of such a crystal varies with its mass or thickness. By depositing the coating directly on the crystal and measuring its oscillation frequency, the coating thickness can be accurately monitored. Let us first consider a single-layer film whose optical thickness (nt) is exactly one-quarter of a wavelength. For light entering the film at normal incidence, the wave reflected from the second surface of the film will be exactly one-half wavelength out of phase with the light reflected from the first surface when they recombine at the first surface, resulting in destructive interference (assuming that there is no phase change by reflection). If the amount of light reflected from each surface is the same, a complete cancellation will occur and no light will be reflected. Thus, if the materials involved are nonabsorbing, all the energy incident on the surface will be transmitted. This is the basis of the “quarter-wave” low-reflection coating which is almost universally used to increase the transmission of optical systems. Since low-reflection coatings reduce reflections, they tend to eliminate ghost images as well as the stray reflected light which reduces contrast in the final image. Before the invention of low-reflection coatings, optical systems which consisted of many separate elements were impractical because of the transmission losses incurred in surface reflections and the frequent ghost images. Even complex lenses were usually limited to only four air-glass surfaces. A magnesium fluoride coating has an additional benefit in that it is actually (when properly applied) a protective coating; the chemical stability of many glasses is enhanced by coating. The reflectivity of a surface coated with one thin film is given by the equation r12  r22  2r1r2 cos X R   (7.21) 1  r12 r22  2r1r2 cos X where X  4n1t1 cos I1 

(7.22)

sin (I0  I1) tan (I0  I1) r1   or  sin (I0  I1) tan (I0  I1)

(7.23)

tan (I1  I2) sin (I1  I2) r2   or  sin (I1  I2) tan (I1  I2)

(7.24)

and is the wavelength of light; t is the thickness of the film; n0, n1, and n2 are the refractive indices of the media; and I0, I1, and I2 are the angles of incidence and refraction. Figure 7.15 shows a sketch of the

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203

film and indicates the physical meanings of the symbols. The sine or tangent expressions for r1 and r2 are chosen depending on the polarization of the incident light as in Eq. 7.19; for unpolarized light, which is composed equally of both polarizations, R is computed for each polarization and the two values are averaged. If we assume nonabsorbing materials, the transmission T equals (1  R). At normal incidence I0  I1  I2  0, and r1 and r2 reduce to n0  n1 r1   n0  n1

(7.25)

n1  n2 r2   n1  n2

(7.26)

Using Eqs. 7.25 and 7.26 for r1 and r2, Eq. 7.21 can be solved for the thickness which yields a minimum reflectance. As the preceding discussion would lead one to expect, this occurs when the optical thickness of the film is one-quarter wavelength, that is, n1t1   4

(7.27)

At normal incidence the reflectivity of a quarter-wave film is thus equal to

冤

(n0n2  n12)  (n0n2  n12)

2

冥

(7.28a)

and the film index which will produce a zero reflectance is n1 

兹苶 n0n2

Figure 7.15 Passage of light ray

through a thin film, indicating the terms used in Eq. 7.21.

(7.28b)

204

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Thus, to produce a coating which will completely eliminate reflections at an air-glass surface, a quarter-wave coating of a material whose index is the square root of the index of the glass is required. Magnesium fluoride (MgF2) with an index of 1.38 is used for this purpose; its ability to form a hard durable film which will withstand weathering and frequently cleaning is the prime reason for its use, despite the fact that its index is higher than the optimum value for almost all optical glasses. Equation 7.28b indicates that the magnesium fluoride, with its index of 1.38, would be an ideal low-reflection coating material for a substrate with an index of 1.382  1.904. Thus it is a much more efficient low-reflection coating for high-index glass than for ordinary glass of a lower index. The measured white light reflection of a low-reflection coating on various index materials is shown in Fig. 7.16. From Eq. 7.21 it is apparent that the reflectivity of a coated surface will vary with wavelength. Obviously a quarter-wave coating for one wavelength will be either more or less than a quarter-wave thick for other wavelengths, and the interference effects will be modified accordingly. Thus a low-reflection coating designed for use in the visible region of the spectrum will have a minimum reflectance for yellow light, and the reflectance for red and blue light will be appreciably higher. This is the cause of the characteristic purple color of singlelayer low-reflection coatings. Figure 7.17 indicates this variation. With more than one layer, more effective antireflection coatings can be constructed. Theoretically, two layers allow the reduction of the reflection to zero, provided that materials of suitable index are available; frequently, three layers are used for this purpose. Such a coating achieves a zero reflectivity at a single wavelength at the

7.16 The measured reflection of white light from an uncoated surface and from a surface coated with a quarterwave MgF2 low-reflection coating, as a function of the index of the base material.

Figure

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205

Figure 7.17 (a) The spectral reflectivity of a single-layer quarter-wave MgF2 coating,

compared with the reflectivity of uncoated glass. The solid curves are for a glass of index 1.69 and the dashed curves are for an index of 1.52. (b) Multilayer coatings. The solid line is a broadband multilayer low-reflection coating. The dashed curve is for a “V-coating,” which can have zero reflectivity at a single wavelength.

expense of a much higher reflectivity on either side. Because of the shape of the reflectivity curve, this is called a V-coating. It is widely used for monochromatic systems, such as those utilizing lasers as light sources. With three or more layers, a broad-band, higher-efficiency, lowreflection coating may be achieved as shown in Fig. 7.17. Such a coating may have two minima as shown, or three, depending on the complexity of the coating design. A typical reflection over the visual spectrum is to the order of 0.25 percent, sometimes with another 0.25 percent lost to scattering and absorption. Thin-film computations

The following equations can be used to calculate the reflection and transmission of an interference coating of any number of layers. The equations can be used at oblique angles and will accommodate absorbing materials. They do require a knowledge of complex arithmetic; if not already familiar with the subject, the interested reader may wish to consult a basic text on complex arithmetic. These equations are the basis of most of the computer programs used in the design and evaluation of thin films. The formulas given here are taken from Peter Berning, in G. Hass (ed.), Physics of Thin Films, vol. 1, Academic, 1963. The reflection and transmission characteristics of a “stack” of several thin films can be expressed in explicit equations; however, their complexity increases rapidly with the number of films, and the following recursion expressions are usually preferable. The physical thickness of each film is represented by tj and the index by nj  Nj  iKj (n is the complex index, N is the ordinary index of refraction, and

206

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K is the absorption coefficient, which is zero for nonabsorbing materials). The angle of incidence within the jth film is j; and the “effective” refractive index is uj  nj cos j or uj  nj/cos j (for light polarized with the electric vector perpendicular to [s], or parallel to [p], the plane of incidence, respectively). Thus, for oblique incidence the calculations are carried out for both polarizations and the results are averaged (assuming the incident light to be unpolarized and to consist of equal parts of each polarization). Since most calculations are carried out at normal incidence (j  0) and for nonabsorbing materials (Kj  0), one may ordinarily use uj  nj  Nj. The subscript notation is j  0 for the substrate, j  1 for the first film, j  2 for the second, etc., j  p  1 for the last film and j  p for the final medium, which is usually air. For each film gj, the effective optical thickness, in radians, is computed from 2nj tj cos j gj  

(7.29)

where is the wavelength of light for which the calculation is made. Starting with E1  E0  1.0 and H1  u0E0  u0, the following equations are applied iteratively at each surface, with the subscript j advancing from j  1 to j  p  1. iHj Ej  1  Ej cos gj   sin gj uj

(7.30)

Hj  1  iujEj sin gj  Hj cos gj

(7.31)

苶 and the other terms have been defined above. Readers where i  兹1 familiar with matrix notation may prefer to manipulate the equivalent matrix form

冢 冣 冢

冣冢 冣

cos gj Ej  1  Hj  1 iuj sin gj

sin gj Ej  (7.32) i cos g Hj j u j When Eqs. 7.30 and 7.31 (or 7.32) have been applied to the entire stack, we have the values of Ep and Hp, which will generally be complex numbers of the form z  x  iy. These are substituted into 1 Hp Ep   Ep    x2  iy2 2 up

(7.33)

1 Hp Ep   Ep    x1  iy1 up 2

(7.34)

冢

冢

冣

冣

and the reflectance of the thin-film system is found from

Optical Materials and Interface Coatings

Ep R  Ep

冨

2

冨

207

(7.35)

where the symbol |z| indicates the modulus of a complex number z, so that |z|  |x  iy|  and

2 兹x苶  y苶2

冨

x1  iy1 R  |z|  x  y   x2  iy2 2

2

2

冨

2

x12  y12   2 x2  y22

If the computation has been for normal incidence through nonabsorbing materials, the transmission is given by T1R

(7.36)

Otherwise, the transmission is given by n0 cos 0 E0 T    np cos p Ep

冨

2

冨

(7.37a)

or n0 cos p E0  T  n cos   Ep p 0

冨

2

冨

(7.37b)

where Eq. 7.37a is used for light polarized with the electric vector perpendicular to [s] and Eq. 7.3b for the electric vector parallel to [p] the plane of incidence. A discussion of the design of multilayer coatings is beyond the scope of this volume; the interested reader may pursue the subject in the references listed at the end of this chapter. By suitable combinations of thin films of different indices and thicknesses a tremendous number of transmission and reflection effects can be created. Among the types of interference coatings which are readily available are long- or shortpass transmission filters, bandpass filters, narrow bandpass (spike filters), achromatic extra-low-reflection coatings as well as the reflection coatings described in the next section. An extremely valuable property of thin-film coatings is their spectral versatility. Once a combination of films has been designed to produce a desired characteristic, the wavelength region can be shifted at will by simply increasing or decreasing all the film thicknesses in proportion. For example, a spike filter designed to transmit a very narrow spectral band at 1 m can be shifted to 2 m by doubling the thickness of each film in the coating. This, of course, is limited by the absorption characteristics of the substrate and the film materials.

208

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The characteristics of a number of typical interference coatings are shown in Fig. 7.18. Note that the wavelength scale is plotted in arbitrary units, with a central wavelength of 1, since (within quite broad limits) the characteristics can be shifted up or down the spectrum as described in the preceding paragraph. Most interference filters are very nearly 100 percent efficient, so that the reflection for a film is equal to one minus the transmission (except in regions where the materials used become absorbing). Since the characteristics of an interference filter depend on the thickness of the films, the characteristics will change when the angle of incidence is changed. This is in great measure due to the fact that the optical path through a film is increased when the light passes through obliquely. For moderate angles the effect is usually to shift the spectral characteristics to a slightly shorter wavelength. The wavelength shift with obliquity is approximated by 0    n

兹苶 n2 s苶 in2

where  is the shifted wavelength at an angle of incidence of , 0 is the wavelength for normal incidence, and n is the “effective index” for the coating stack (n is typically in the range of 1.5 to 1.9 for most coatings).

Figure 7.18 Transmission of typical evaporated interference filters plotted

against wavelength in arbitrary units. (Upper left) Short-pass filter (note that dashed portion of curve must be blocked by another filter if low long wavelength transmission is necessary). (Upper right) Long-pass filter. (Lower left) Bandpass filter. (Lower right) Narrow bandpass (spike) filter.

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209

Coatings also shift wavelength effects with temperature; this shift is to the order of one- or two-tenths of an angstrom per degree Celsius. Coatings consisting of a few layers are for the most part reasonably durable and can withstand careful cleaning. However, coatings consisting of a great number of layers (and coatings consisting of 50 or more layers are occasionally used) tend toward delicacy, and must be handled with due respect. Some multilayer coatings are quite effective polarizers when used obliquely (and as such, are occasionally responsible for “mysterious” happenings). This is notably true in systems using linearly polarized laser beams. One must also exercise care in photometric or radiometric applications (e.g., spectrophotometers), since polarization effects can introduce significant errors. 7.10

Reflectors

Although polished bulk metals are occasionally used for mirror surfaces, most optical reflectors are fabricated by evaporating one or more thin films on a polished surface, which is usually glass. Obviously the interference filters described in the preceding section can be used as specialpurpose reflectors in instances where their spectral characteristics are suitable. However, the workhorse reflector material for the great majority of applications is an aluminum film deposited on a substrate by evaporation in vacuum. Aluminum has a broad spectral band of quite high reflectivity and is reasonably durable when properly applied. Almost all aluminum mirrors are “overcoated” with a thin protective layer of either silicon monoxide or magnesium fluoride. This combination produces a first-surface mirror which is rugged enough to withstand ordinary handling and cleaning without undue scratching or other signs of wear. The spectral reflectance characteristics of several evaporated metal films are shown in Fig. 7.19. With the exception of the curve for rhodium, the reflectivities given here can seldom be attained for practical purposes; the silver coating will tarnish and the aluminum film will oxidize, so that the reflectances tend to decrease with age, especially at shorter wavelengths. The high reflectivity of silver is only useful when the coating can be properly protected. Figure 7.20 indicates the variety of characteristics which are available in commercial aluminum mirrors. A run-of-the-mill protected aluminum mirror can be expected to have an average visual reflectance of about 88 percent. Two, four, or more interference films may be added to improve the reflectance where the additional cost can be accepted. This enhanced reflectivity within the bandpass of the mirror is obtained at the expense of a lowered reflectivity on either side, as can be seen from the dashed curve in Fig. 7.20.

210

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Figure 7.19 Spectral reflectance for evaporated metal films on glass. Data repre-

sents new coatings, under ideal conditions.

Figure 7.20 Spectral reflectance of aluminum mirrors. The solid curves are for

aluminum films with various types of thin film overcoatings—either for protection or for increased reflectivity. The dashed line is an extra-high-reflectance multilayer coating. All coatings shown are commercially available.

Dichroics and semireflecting mirrors constitute another class of reflector. Both are used to split a beam of light into two parts. A dichroic reflector splits the light beam spectrally, in that it transmits certain wavelengths and reflects others. A dichroic reflector is often used for heat control in projectors and other illuminating devices. A hot mirror is a dichroic which transmits the visible region of the spectrum and reflects the near infrared. A cold mirror does just the reverse, in that it transmits the infrared and reflects the visible. For example, a cold mirror introduced into the optical path will allow undesired heat in the form of infrared radiation to be removed from

Optical Materials and Interface Coatings

211

the beam by transmitting it to a heat dump. These mirrors have the advantage over heat-absorbing filter glass in that they do not themselves get hot and thus do not require a fan for cooling. A semireflecting mirror is, nominally at least, spectrally neutral; its function is to divide a beam into two portions, each with similar spectral characteristics. Figure 7.21 shows the characteristics of a variety of these partial reflectors. 7.11 Reticles A reticle is a pattern used at or near the focus of an optical system, such as the cross hairs in a telescope. For a simple cross-hair pattern, fine wire or spider (web) hair is occasionally used, stretched across an open frame. However, a pattern which is supported on a glass (or other material) substrate offers considerably more versatility, and most reticles, scales, divided circles, and patterns are of this type.

Figure 7.21 Characteristics of partial reflectors. (a) Multilayer “neutral” semi-

reflectors (efficiency better than 99 percent). (b) Dichroic multilayer reflectors—blue, green, red, and yellow reflection. (c) Visual efficiency of aluminum semireflectors. (d) Visual efficiency of chrome semireflectors.

212

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The simplest type of reticle is produced by scribing, or scoring, the glass surface with a diamond tool. A line produced this way, while not opaque, modifies the glass sufficiently so that under the proper type of illumination the line will appear dark. Where clear lines in an opaque background are desired, the glass can be coated with an opaque coating, such as evaporated aluminum, and the lines scribed through the coating with a diamond or hardened steel tool, depending on the type of line desired. Scribing produces very fine lines. Another old technique is to etch the substrate material. A waxy resist is coated on the substrate and the desired pattern cut through the resist. The exposed portion of the substrate is then etched (with hydrofluoric acid in the case of glass) to produce a groove in the material. The groove can be filled with titanium dioxide (white), or lamp black in a waterglass medium, or evaporated metal. Etched reticles are durable and have the advantage that they can be edge-lighted if illumination is necessary. Any substrate that is readily etched can be used. This process is used for many military reticles and also for accurate metrology scales on steel. The most versatile processes for production of reticles are based on the use of a photoresist, or photosensitive material. Photoresists are exposed like a photographic emulsion, either by contact printing through a master or by photography. However, when the photoresist is “developed,” the exposed areas are left covered with the resist and the unexposed areas are completely clear. Thus, an evaporated coating of any of a number of metals (aluminum, chrome, inconel, nichrome, copper, germanium, etc.) can be deposited over the resist. In the clear areas the coating adheres to the substrate; when the resist is removed, it carries away the coating deposited upon it, leaving a durable pattern which is an exact duplicate of the master. The precision, versatility, ruggedness, and suitability for mass production of this technique have earned it a prominent place in the field of reticle manufacture. The photoresist technique may also be combined with etching, where the material to be etched is either a metal substrate or an evaporated metal film. Where the reticle pattern must be nonreflecting, the glue silver process or the black-print process is used. The technique is similar to that used in producing the photoresist pattern, except that the photosensitive material is opaque. The clear areas are free of emulsion. Glue silver reticles are fragile but capable of very high resolution of detail. The black-print process is more durable. Occasionally an extremely high resolution photographic emulsion is used for a reticle pattern; however, the presence of emulsion in the clear areas of the pattern is ordinarily a drawback.

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213

The following tabulation indicates the resolution and accuracy possible with these techniques. These figures represent the highest level of quality that reticle manufacturers are capable of at the present time; if cost is a factor, one is well advised to lower one’s requirements an order of magnitude or so below the levels indicated here.

Method Scribing Etch (and fill) Photo-resist (evaporated metal) Glue silver Black print Emulsion

7.12

Finest line width, in

Dimensional repeatability, in

Minimum figure height, in

0.00001 0.0002–0.0004

±0.00001 ±0.0001

0.004

0.001–0.002 0.00003–0.0002 0.001 0.00005–0.0001

±0.00005 ±0.00005–0.0005 ±0.0001 ±0.00005

0.002 0.002 0.005 0.001

Cements and Liquids

Optical cements are used to fasten optical elements together. Two main purposes are served by cementing: the elements are held in accurate alignment with each other independent of their mechanical mount, and the reflections from the surfaces (especially those from TIR; see Sec. 4.6) are largely eliminated by cementing. Ordinarily the layer of cement used is extremely thin and its effect on the optical characteristics of the system can be totally neglected; some of the newer plastic cements, designed to withstand extremes of temperature, are used in thicknesses of a few thousandths of an inch (which could affect the performance of an optical system under critical conditions where the light rays have large slopes). Canada balsam is made from the sap of the balsam fir. It is available in a liquid form (dissolved in xylol) and in stick or solid form. Elements to be cemented are cleaned and placed together on a hot plate. When the elements are warm enough to melt the balsam, the stick is rubbed on the lower element. The upper element is replaced and the excess cement and any entrapped air bubbles are worked out by oscillating or rocking the upper element. The elements are then placed in an alignment fixture to cool. Balsam cement has an index of refraction of about 1.54 and a V-value of about 42. These are conveniently midway between the refractive characteristics of crown and flint glasses. Unfortunately, Canada balsam will not withstand high or low temperatures. It softens when heated and splits at low temperatures and is thus unsuited for rigorous thermal environments. Balsam is rarely used today.

214

Chapter Seven

A great number of plastic cements have been developed to withstand extremes of both temperature and shock. For the most part, these are thermosetting (heat-curing) or ultraviolet light-curing plastics, although a few thermoplastic (heat-softening) materials are used. Cements are available which will withstand temperatures from 82°C down to 65°C without failure when properly used. In general the thermosetting cements are supplied in two containers (sometimes refrigerated), one of which contains a catalyst which is mixed into the cement prior to use. A drop of cement is placed between the elements to be cemented, the excess cement and air bubbles are worked out, and the elements are placed in a fixture or jig for a heating cycle which cures the cement. Once the cement has set, it is exceedingly difficult to separate the components; the customary technique is to shock them apart by immersion in hot (150 to 200°C) castor oil. The index of refraction of plastic cements ranges from 1.47 to 1.61, depending on the type, with most cements falling between 1.53 and 1.58 with a Vvalue between 35 and 45. Epoxies and methacrylates are widely used. Because of the variety of types and characteristics which are available, one should consult the manufacturer’s literature for specific details regarding any given cement. A rarely used method of fastening optical elements together is by what is called optical contact. Both pieces must be scrupulously cleaned (often the final cleaning is with a cloth slightly stained with polishing rouge) and laid together. If the surface shapes match well enough, as the air is pressed out from between the pieces, a molecular attraction will cause them to adhere in a surprisingly strong bond, which will withstand a force of about 95 lb/in2. Usually the only way properly contacted surfaces can be separated is by heating one of them and allowing thermal expansion to break the contact (it often breaks the glass as well). Occasionally, soaking in water will separate the pieces. Optical liquids are used primarily for microscope immersion fluids and for use in index measurement (in critical-angle refractometers). For microscopy, water (nd  1.33), cedar oil (nd  1.515), and glycerin (ultraviolet n  1.45) are frequently utilized. For refractometers alpha-bromonaphthalene (n  1.66) is the most commonly used liquid. Methylene iodide (n  1.74) is used for high index measurement (since the liquid index must be larger than that of the sample to avoid total internal reflection back into the sample). Bibliography Note: Titles preceded by an asterisk (*) are out of print. American Institute of Physics Handbook, 3d ed., New York, McGrawHill, 1972.

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Ballard, S., K. McCarthy, and W. Wolfe, Optical Materials for Infrared Instrumentation, Univ. of Michigan, 1959 (Supplement, 1961). Barnes, W., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 7, New York, Academic, 1979 (reflective materials). Baumeister, P., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (coatings). Bennett, J. M., “Polarization,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 5. Bennett, J. M., “Polarizers,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 3. Berning, P., in Hass (ed.), Physics of Thin Films, vol. 1, New York, Academic, 1963 (calculations). *Conrady, A., Applied Optics and Optical Design, Oxford, 1929. (This and vol. 2 were also published by Dover, New York.) Dobrowolski, J., “Optical Properties of Films and Coatings,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 42. Dobrowolski, J., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978 (coatings). Driscoll, W. (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. *Hackforth, H., Infrared Radiation, New York, McGraw-Hill, 1960. Handbook of Chemistry and Physics, Chemical Rubber Publishing Co., published annually. *Hardy, A., and F. Perrin, The Principles of Optics, New York, McGraw-Hill, 1932. Hass, G., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1975 (mirror coatings). *Heavens, O., Optical Properties of Thin Films, London, Butterworth’s, 1955. Herzberger, M., Modern Geometrical Optics, New York, Interscience, 1958. *Holland, L., Vacuum Deposition of Thin Films, New York, Wiley, 1956. Jacobs, S., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 10, San Diego, Academic, 1987 (dimensional stability). *Jacobs, D., Fundamentals of Optical Engineering, New York, McGraw-Hill, 1943. Jacobson, R., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (projection screens). *Jamieson, J., et al., Infrared Physics and Engineering, New York, McGraw-Hill, 1963. Jenkins, F., and H. White, Fundamentals of Optics, 4th ed., New York, McGraw-Hill, 1976. Kreidl, N., and J. Rood, in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (materials).

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Lytle, J. D., “Polymetric Optics,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 34. Macleod, H., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 10, San Diego, Academic, 1987 (coatings). Macleod, H., Thin Film Optical Filters, 2d ed., New York, McGrawHill, 1988. Meltzer, R., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (polarization). Moore, D. T., “Gradient Index Optics,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 9. Palmer, J. M., “The Measurement of Transmission, Absorption, Emission and Reflection,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 25. Paquin, R. A., “Properties of Metals,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 35. Parker, C., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 7, New York, Academic, 1979 (refractive materials). Photonics Buyers Guide, Optical Industry Directory, Laurin Publishers, Pittsfield, MA (published annually). Pompea, S. M., and R. P. Breault, “Black Surfaces for Optical Systems,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 37. Rancourt, J., Optical Thin Films, New York, McGraw-Hill, 1987. Scharf, P., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (filters). *Strong, J., Concepts of Classical Optics, New York, Freeman, 1958. Thelen, A., Design of Optical Interference Coatings, New York, McGraw-Hill, 1988. Tropf, W. J., M. Thomas, and T. J. Harris, “Properties of Crystals and Glasses,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 33. *Vasicek, A., Optics of Thin Films, Amsterdam, North Holland, 1960. Welham, B., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 7, New York, Academic, 1979 (plastics). Wolfe, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGrawHill, 1978 (materials). Wolfe, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, D.C., Office of Naval Research, 1985 (materials). Exercises 1 (a) What is the transmission of a stack of three thin plane parallel plates of glass (n  1.5) at normal incidence?

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217

(b) What percentage of the incident light is transmitted directly (i.e., without any intervening reflections)? ANSWER:

(a) 80 percent, (b) (0.96)6  78 percent

2 If a 1-cm thickness of a material transmits 85 percent and 2-cm thickness transmits 80 percent, (a) what percentage will a 3-cm thickness transmit? (b) What is the absorption coefficient of the material? (Neglect all multiple reflections.) ANSWER:

(a) 75.3 percent; (b) 0.06062 cm1

3 Determine the coefficients for the dispersion equations given in Section 7.1 for one of the optical glasses listed in Fig. 7.4. Evaluate the accuracy of the equations by comparing the index values given by the equations with those listed in the table (for wavelengths not used in determining the constants). 4 Using the spectral transmission curves of Fig. 7.10, plot the spectral transmission which would result from a combination of filters (c) and (f). 5 Plot, in the manner of Fig. 7.14, the curve of reflection against angle of incidence for a single surface of glass (n  1.52) coated with a quarter wavelength thickness of magnesium fluoride (n  1.38).

Chapter

8 Radiometry and Photometry

8.1

Introduction

In concept, both radiometry and photometry are quite straightforward; however, both have been cursed with a jungle of often bewildering terminology. Radiometry deals with radiant energy (i.e., electromagnetic radiation) of any wavelength. Photometry is restricted to radiation in the visible region of the spectrum. The basic unit of power (i.e., rate of transfer of energy) in radiometry is the watt; in photometry, the corresponding unit is the lumen, which is simply radiant power as modified by the relative spectral sensitivity of the eye (Fig. 5.10) per Eq. 8.18. Note that watts and lumens have the same dimensions, namely energy per time. All radiometry must take into account the variation of characteristics with wavelength. Examples are the spectral variation of emission, the variation of transmission of the atmosphere and optics with wavelength, and the differences in detector and film response with wavelength. A convenient way to deal with this is to multiply, wavelength by wavelength, all such factors together so as to arrive at one unified spectral weighting function. Thus, all radiometry is spectrally weighted and it should be apparent that photometry is simply one particular spectral weighting. See Sec. 8.9. The principles of radiometry and photometry are readily understood when one thinks in terms of the basic units involved, rather than the special terminology which is conventionally used. The next five sections will discuss radiation in terms of watts; the reader should

219

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remember that the discussion is equally valid for photometry, if lumens are read for watts. 8.2 The Inverse Square Law; Intensity Consider a hypothetical point (or “sufficiently” small) source of radiant energy, which is radiating uniformly in all directions. If the rate at which energy is radiated is P watts, then the source has a radiant intensity J of P/4 watts per steradian,* since the solid angle into which the energy is radiated is a sphere of 4 steradians. Of course there are no truly “point” sources and no practical sources which radiate uniformly in all directions, but if a source is quite small relative to its distance, it can be treated as a point, and its radiation, in the directions in which it does radiate, can be expressed in watts per steradian. If we now consider a surface which is S cm from the source, then 1 cm2 of this surface will subtend 1/S2 steradians from the source (at the point where the normal from the source to the surface intersects the surface, if S is large). The irradiance H on this surface is the incident radiant power per unit area and is obtained by multiplying the intensity of the source in watts per steradian by the solid angle subtended by the unit area. Thus, the irradiance is given by 1 H  J 2 S

(8.1)

The units of irradiance are watts per square centimeter (W/cm2). Equation 8.1 is, of course, the “inverse square” law, which is conventionally stated: the illumination (irradiance) on a surface is inversely proportional to the square of the distance from the (point) source. Thus, if our uniformly radiating point source emits energy at a rate of 10 W, it will have an intensity J  10/4  0.8 W ster1, and the radiation falling on a surface 100 cm away would be 0.8  104 W/cm2, or 80 W/cm2. If the surface is flat, the irradiance will, of course, be less than this at points where the radiation is incident at an angle, since the solid angle subtended by a unit of area in the surface will be reduced. From Fig. 8.1 it can be seen that the source-to-surface distance is increased to S/cos  and that the effective area (normal to the *A steradian is the solid angle subtended (from its center) by 1/4 of the surface area of a sphere. Thus, a sphere subtends 4 (12.566) steradians from its center; a hemisphere subtends 2 steradians. The size of a solid angle in steradians is found by determining the area of that portion of the surface of a sphere which is included within the solid angle and dividing this area by the square of the radius of the sphere. For a small solid angle, the area of the included flat surface normal to the “central axis” of the angle can be divided by the square of the distance from the surface to the apex of the angle to determine its size in steradians. One can visualize a steradian as a cone with an apex angle of about 65.5°, or 3283 square degrees.

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Figure 8.1 Geometry of a point

source irradiating a plane, showing that irradiance (or illumination) varies with cos3 .

direction of the radiation) is reduced by a cos  factor. Thus, the solid angle subtended, and the irradiance, are reduced by a cos3  factor. 8.3 Radiance and Lambert’s Law An extended source, that is, one whose dimensions are significant, must be treated differently than a point source. A small area of the source will radiate a certain amount of power per unit of solid angle. Thus, the radiation characteristics of an extended source are expressed in terms of power per unit solid angle per unit area. This is called radiance; the usual units for radiance are watts per steradian per square centimeter (W ster1 cm2) and the symbol is N. Note that the area is measured normal to the direction of radiation, not in the radiating surface. Most extended sources of radiation follow, at least approximately, what is known as Lambert’s law of intensity, J  J0 cos

(8.2)

where J is the intensity of a small incremental area of the source in a direction at an angle  from the normal to the surface, and J0 is the intensity of the incremental area in the direction of the normal. For example, a heated metal disk with a total area of 1 cm2 and a radiance of 1 W ster1 cm2 will radiate 1 W/ster in a direction normal to its surface. In a direction 45° to the normal, it will radiate only 0.707 W/ster (cos 45°  0.707). Notice that although radiance is given in terms of watts per steradian per square centimeter, this should not be taken to mean that the radiation is uniform over a full steradian or over a full square centimeter. Consider a source consisting of a 0.1-cm square incandescent

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filament in a 20-cm-diameter envelope. Assume that the bulb is painted so that only a 1-cm square transmits energy, and that the source radiates one-fiftieth of a watt through this square. (We assume, for convenience, that the radiation intercepted by the painted envelope is thereby totally removed from consideration.) Now the filament has an area of 0.01 cm2 and is radiating 0.02 W into a solid angle of (approximately) 0.01 steradian. Therefore, it has a radiance of 200 W ster1 cm2, but only within the solid angle subtended by the window! Outside this angle the radiance is zero. This concept of radiance over a limited angle becomes important in dealing with the radiance of images and must be thoroughly understood. There are several interesting consequences of Lambert’s law that are worthy of consideration, not only for their own sake but because they illustrate the basic techniques of radiometric calculations. The radiance of a surface is conventionally taken with respect to the area of a surface normal to the direction of radiation. It can be seen that, although the emitted radiation per steradian falls off with cos  according to Lambert’s law, the “projected” surface area falls off at exactly the same rate. The result is that the radiance of a Lambertian surface is constant with respect to . In visual work the quantity corresponding to radiance is brightness, and the above is readily demonstrated by observing that the brightness of a diffuse source is the same regardless of the angle from which it is viewed. 8.4 Radiation into a Hemisphere Let us determine the total power radiated from a flat diffuse source into a hemisphere. If the source has a radiance of N W ster1 cm2, one might expect that the power radiated into a hemisphere of 2 steradians would be 2N W/cm2. That this is twice too large is readily shown. With reference to Fig. 8.2, let A represent the area of a small source with a radiance of N W ster1 cm2 and an intensity of J  J0 cos   NA cos  W/ster. The incremental ring area on a hemisphere of radius R has an area of 2R sin  R d and thus subtends (from A) a solid angle of 2R2 sin  d/R2  2 sin  d steradians. The radiation intercepted by this ring is the product of the intensity of the source and the solid angle, or dP  J 2 sin  d  2NA sin  cos  d

(8.3)

Integrating to find the total power radiated into the hemisphere from A, we get

冕

/2

P

0

冤

sin2  2NA sin  cos  d  2NA  2

冥

/2 0

 NA watts (8.4)

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Figure 8.2 Geometry of a lambertian

source radiating into a hemisphere.

Dividing by A to get watts emitted per square centimeter of source, we find the radiation into the 2 steradian of the hemisphere to be N W/cm2, not 2N. This is the basic relationship between radiance and the power emitted from the surface.

8.5 Irradiance Produced by a Diffuse Source It is frequently of interest to determine the irradiance produced at a point by a lambertian source of finite size. Referring to Fig. 8.3, assume that the source is a circular disk of radius R and that we wish to determine the irradiance at some point X which is a distance S from the source and is on the normal through the center of the source. (Note that we will determine the irradiance on a plane parallel to the plane of the source.) The radiant intensity of a small element of area dA in the direction of point X is given by Eq. 8.2 as J  J0 cos   N dA cos  where N is the radiance of the source. Since the distance from dA to X is S/cos , and the radiation arrives at an angle , the incremental irradiance at X produced by dA is cos3  N dA cos4   dH  J0 cos    S2 S2

冤

冥

(8.5)

The same irradiance is produced by each incremental area making up a ring of radius r and a width dr, so that we can substitute the area of the ring, 2r dr, for dA in Eq. 8.5 to get the incremental irradiance from the ring. 2r dr N cos4  dH   S2

(8.6)

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Figure 8.3 Geometry of a circu-

lar source irradiating point X.

To simplify the integration, we substitute r  S tan  dr  S sec2  d into Eq. 8.6 to get 2S tan S sec2  dN cos4  dH   S2  2N tan  cos2  d  2N sin  cos  d Integrating to determine the irradiance from the entire source, we get H

冕

 0

冤

sin2  2N sin  cos  d  2N  2

H  N sin 2  m2 watt/cm2

冥

 0

(8.7)

where H is the irradiance produced at a point by a circular source of radiance N W ster1 cm2 which subtends an angle of 2m from the point (when the point is on the “axis” of the source). Note well that m is the angle defined by the source diameter. Unfortunately noncircular sources do not readily yield to analysis. However, small noncircular sources may be approximated with a fair degree of accuracy by noting that the solid angle subtended by the source from X is sin2    2 (1  cos )  2  (1  cos ) and for small values of , cos  approaches unity and    sin2 

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Thus, if the angle subtended by the source is moderate, we can substitute into Eq. 8.7 and write H  N

(8.8)

If the point X does not lie on the “axis” (the normal through the center of the circular source), then the irradiance would be subject to the same factors outlined in the discussion of the “cosine-fourth” rule in Sec. 6.7. Thus, if the line from the point X to the center of the circle makes an angle  to the normal, the irradiance at X is given by H  H0 cos4 

(8.9)

where H0 is the irradiance along the normal given by Eq. 8.7 or 8.8 and H is the irradiance at X (measured in a plane parallel to the source). (See the note in Example A regarding the inaccuracy of the cosinefourth rule when the angles  and  are large.) It is apparent that Eqs. 8.8 and 8.9 may be used in combination to calculate the irradiance produced by any conceivable source configuration, to whatever degree of accuracy that time (or patience) allows. 8.6 The Radiometry of Images; The Conservation of Radiance When a source is imaged by an optical system, the image has a radiance, and it may be treated as a secondary source of radiation. However, one must always keep in mind that the radiance of an image differs from the radiance of an ordinary source in that the radiance of an image exists only within the solid angle subtended from the image by the clear aperture of the optical system. Outside of this angle, the radiance of the image is zero. Figure 8.4 illustrates an aplanatic optical system imaging an incremental area A of a lambertian source at A′. We will consider the radiance of the image at A′ formed through a generalized incremental area P in the principal surface of the optical system. (Since the system is aplanatic, that is, free of coma and spherical aberration, the principal “planes” are spherical surfaces and are centered on the object and image.) The radiance of the source is N W ster1 cm2 and the projected area of A in the direction  is A cos  cm2. The solid angle subtended by incremental area P from A is P/S2, where S is the distance from the object to the first principal surface. Therefore, the radiant power intercepted by area P is P Power  N 2 A cos  watts S

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Figure 8.4 Illustrates an aplanatic optical system imaging an

incremental source area A at A′.

This radiation is imaged by the optical system at area A′, into a (projected) area A′ cos ′, through a solid angle P′/S ′ 2. Thus, the radiance at A′ is given by S′2 P   N′  TN 2 A cos  watt ster1 cm2 P ′A′ cos ′ S

冤

冥

where T is the transmission of the optical system. Now we note that the incremental areas A and A′ are related by the laws of first-order optics, and, if both are in media of the same index, AS′ 2  A′S 2. Further, the principal surfaces are unit images of each other; taking the tilts of the surfaces into account, we get P cos   P′ cos ′. Making these substitutions and clearing, we find that the radiance of the image is equal to that of the object times the transmission of the system, or (8.10)

N′  TN

This fundamental relationship can be restated with slightly different emphasis: the radiance of an image cannot exceed that of the object.* *This statement and Eqs. 8.10 and 8.11 are subject to the condition that both object and image lie in media of the same index of refraction. When the media have different indices, the image radiance and irradiance are multiplied by the factor (ni/n0)2, where ni and n0 are the refractive indices of the image media and object media, respectively. Thus, Eqs. 8.10 and 8.11 become ni 2 (8.10a) N′  TN  n0

冢 冣

ni H  TN  n0

2

ni  TN  n0

2

冢 冣

冢 冣

 sin2 ′ 

(8.11a)

The factor (ni/n0) is introduced by the use of An02S′2  A′ni2S2 in place of AS′2  A′S2 in the derivation of Eq. 8.10; both equalities are derived from the optical invariant relationship hnu  h′n′u′ (Eq. 2.55).

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At first consideration the conservation of radiance (or brightness) seems quite counterintuitive. Ordinarily, the solid angle of radiation accepted by an optical system from a source is quite small, as is the fraction of the total power which passes through the lens and forms the image. It is difficult to accept that the image formed by this small fraction of the source power will have the same radiance as does the source. We can easily demonstrate this, using only the first-order optics from Chap. 2. Let us assume a small source of radiance N with an area A. The source thus has an intensity of AN. The source is imaged by an optical system with an area P which is located a distance S from the source. The solid angle subtended by the lens from the source is thus P/S2, and the power intercepted by the lens and formed into the image is ANP/S2. The lens will form an image with a magnification M, and the area of the image will thus be AM2. The image distance will be MS, and the solid angle subtended by the lens from the image will be P/M2S2 ster. Thus the power in the image (ANP/S2) is spread over the image area (AM2) and exists only over the solid angle (P/M2S2). The image radiance is power per unit area per solid angle; combining the expressions above, we get (neglecting any transmission losses) Image radiance  power/area solid angle  (ANP/S 2) / (AM 2) (P/M2S 2) We can cancel A, P, S, and M, leaving us with Image radiance  N (the object radiance) which is a statement of the conservation of radiance (or brightness). By the application of exactly the same integration technique used in Sec. 8.5, it can be shown that the irradiance produced in the plane of an image is given by H  TN sin2 ′ watt/cm2  TN (for small angles)

(8.11)

where T is the system transmission, N (W ster1 cm2) is the object radiance, and ′ is the half angle subtended by the exit pupil of the optical system from the image. Small or noncircular exit pupils and cylindrical lens systems can be handled by substituting the solid angle  for  sin2 ′ (just as in Eq. 8.8); image points off the optical axis are subject to the cosine-fourth law in addition to any losses due to vignetting (Eq. 8.9 and Sec. 6.7). The similarity between the equations for the irradiance produced by a diffuse source and by an optical system makes it apparent that, when it is viewed from the image point, the aperture of the optical system takes on the radiance of the object it is imaging. This is an

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extremely useful concept; for radiometric purposes, a complex optical system can often be treated as if it consisted solely of a transmission loss and an exit pupil with the same radiance as the object. Similarly, when an optical system produces an image of a source, the image can be treated as a new source of the same radiance (less transmission losses). Of course, the direction that radiation is emitted from the image is limited by the aperture of the system. When an object is so small that its image is a diffraction pattern (Airy disk), then the preceding techniques, which apply to extended sources, cannot be used. Instead, the power intercepted by the optical system, reduced by transmission losses, is spread into the diffraction pattern. To determine the irradiance (or the radiance) of the image, we note that 84 percent of the power intercepted and transmitted by the lens is concentrated into the central bright spot (the Airy disk). A precise determination of irradiance requires that one integrate the relative irradiance-times-area product over the central disk and equate this to 84 percent of the image power. If P is the total power in the Airy pattern, H0 the irradiance at the center of the pattern, and z the radius of the first dark ring, a numerical integration of Eq. 6.18 over the central disk yields 0.84P  0.72H0 z 2 Rearranging and substituting the value of z given by Eq. 6.20, we get NA 2 P H0  1.17 2  P  z

冢 冣

where is the wavelength and NA is n′ sin U′, the numerical aperture. The irradiance for points not at the center of the pattern is then found by Eq. 6.18. Note that the preceding assumes a circular aperture; for rectangular apertures, the process would be based on Eq. 6.16. Example A

In Fig. 8.5, A is a circular source with a radiance of 10 W per ster per cm2 radiating toward plane BC. The diameter of A subtends 60° from point B. The distance AB is 100 cm and the distance BC is 100 cm. An optical system at D forms an image of the region about point C at E. Plane BC is a diffuse (lambertian) reflector with a reflectivity of 70 percent. The optical system (D) has a 1-in-square aperture and the distance from D to E is 100 in. The transmission of the optical system is 80 percent. We wish to determine the power incident on a 1-cm square photodetector at E. We begin by determining the irradiance at B, using Eq. 8.7; the source radiance is 10 W ster1 cm2 and the half angle  is 30°, giving

冢 冣  7.85 W/cm

1 HB  N sin 2    10  2

2

2

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229

Figure 8.5 Example A.

Since angle BAC is 45°, we can find the irradiance at C from Eq. 8.9, noting that cos 45° is 0.707 HC  HB cos4 45°  7.85  (0.707)4  1.96 W/cm2 (Note that the cosine-fourth effect derived in Sec. 6.7 included one cosine term which was approximate; its accuracy depended on the distance from the pupil to the image surface being much larger than the pupil diameter. In Example A this approximation is quite poor. P. Foote, in the Bulletin of the Bureau of Standards 12, 583 (1915), gave the following expression for the irradiance, which is accurate even when the source is large compared with the distance. N H  2

冤

(1  tan2   tan2 ) 1   [tan4   2 tan2 (1  tan2 )  1/cos4]1/2

冥

If we compare the irradiance from this equation with that from Eqs. 8.7 and 8.8 for the angles  and  from Example A, we find that this irradiance is 42 percent greater than the cosine-fourth result. This is, of course, a rather extreme case.) It is now necessary to determine the radiance of the surface at C. The diffuse surface at C reradiates 70 percent of the incident 1.96 W/cm2 into a full hemisphere; the total power reradiated is thus 1.37 W/cm2. In Sec. 8.4 it was shown that a source of radiance N radiated N W/cm2 into a hemisphere. Thus the radiance at point C is given by

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Chapter Eight

0.7  1.96 RH 1.37 NC        0.44 W ster1 cm2    The irradiance at E can now be determined from Eq. 8.11, noting that the solid angle subtended by the aperture of the lens system is 1/(100)2, or 104 ster, and substituting this for  sin2  in Eq. 8.11, HE  TDNC sin2   TD NC  0.8  0.44  104  0.35  104 W/cm2 Since the photodetector at E has an area of 1 cm2, the radiant power falling on it is just 0.35  104 W, or 35 W. 8.7 Spectral Radiometry In the preceding discussion, no mention has been made of the spectral characteristics of the radiation. It is apparent that every radiant source has some sort of spectral distribution of its radiation, in that it will emit more radiation at certain wavelengths than others. For many purposes, it is necessary to treat intensity (J), irradiance (H), radiance (N), etc. (in fact, all the quantities listed in Fig. 8.6) as functions of wavelength. To do this we refer to the above quantities per unit interval of wavelength. Thus, if a source emits 5 W of radiant power in the spectral band between 2 and 2.1 m, it emits 50 W per micrometer (W/m) in this region of the spectrum. The standard symbol for this type of quantity is the symbol given in Fig. 8.6 subscripted with a , and the name is preceded by “spectral.” For example, the symbol for spectral radiance is N and its units are watts per steradian per square centimeter per micrometer (W ster1 cm2 m1).

Figure 8.6 Radiometric terminology. The names, symbols, descriptions, and preferred

units for quantities in radiometric work.

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231

In many applications it is absolutely necessary to take the spectral characteristics of sources, detectors, optical systems, filters, and the like into account. This is accomplished by integrating the particular radiation product function over an appropriate wavelength interval. Since most spectral characteristics are not ordinary functions, the process of integration is usually numerical, and thus laborious. As a brief example, suppose that the irradiance in an image is desired. The spectral radiance of the object can be described by some function N( ) and the transmission of the atmosphere, the optical system, and any filters can be combined in a spectral transmission function T( ). Equation 8.11 will give the irradiance of the image (for any given wavelength); for use over an extended wavelength interval, we must write H

冕

2

冕

2

T( ) N( ) sin2  d   sin2 

1

T( ) N ( ) d W/cm2

(8.12)

1

where 1 and 2, the limits of the integration, may be zero and infinity, but are usually taken as real wavelengths which encompass the region of interest. In practice, it is usually necessary to perform the integration numerically; this process is represented (for this particular example) by the summation: 2

H   sin2 冱

T( ) N( ) W/cm2

(8.13)

 1

The spectral response of a detector is included in a calculation in the same manner. For example, the effective power falling on a detector with an area of A and a relative spectral response R( ), when the detector is located in the image plane of the system above, would be (provided that the image completely covered the detector) P  A sin2 

冕

2

R( ) T( ) N( ) d W

1

8.8 Blackbody Radiation A perfect blackbody is one which totally absorbs all radiation incident upon it. The radiation characteristics of a heated blackbody are subject to known laws, and since it is possible to build a close approximation to an ideal blackbody, a device of this type is a very useful standard source for the calibration and testing of radiometric instruments. Further, most sources of thermal radiation, i.e., sources which radiate because they are heated, radiate energy in a manner which can be readily described in terms of a blackbody emitting through a filter, making it possible to use the blackbody radiation laws as a starting point for many radiometric calculations.

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Planck’s law describes the spectral radiant emittance of a perfect blackbody as a function of its temperature and the wavelength of the emitted radiation. C1 (8.14) W   5 C2/ T  1) (e where W  the radiation emitted into a hemisphere by the blackbody in power per unit area per wavelength interval (W cm2 m1)  the wavelength (m) e  the base of natural logarithms (2.718…) T  the temperature of the blackbody in Kelvin (K  °C  273) C1  a constant  3.742  104 when area is in square centimeters and wavelength in micrometers C2  a constant  1.4388  104 when square centimeters and micrometers are used Figure 8.7 indicates the shape of the curve of W plotted against wavelength. Note that the spectral radiance (N ) is given by W /. If we integrate Eq. 8.14, we can obtain the total radiation at all wavelengths. The resulting equation is known as the StefanBoltzmann law, WTOT  5.67  1012 T 4 W/cm2

(8.15)

and indicates that the total power radiated from a blackbody varies as the fourth power of the absolute temperature. If we differentiate Planck’s equation (8.14) and set the result equal to zero, we can determine the wavelength at which the spectral emittance (W ) is a maximum and also the amount of W at this wavelength. Wien’s displacement law gives the wavelength for maximum W as max  2897.8T1 m

(8.16)

W , max  1.286  1015T 5 W/cm2 m1

(8.17)

and W at max as

Notice that the higher the temperature, the shorter the wavelength at which the peak occurs and that W at the peak varies as the fifth power of the absolute temperature. Before the advent of the electronic calculator, Planck’s equation was very awkward to use and for this reason a number of tables, charts,

233

Figure 8.7 Spectral distribution of blackbody radiation (normalized).

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Chapter Eight

and slide rules are available which allow the user to simply look up the values of W for the appropriate temperature and wavelength. Figure 8.7 may be used for this purpose when the precision required is relatively modest. The use of Fig. 8.7 is quite simple: First the total energy (WTOT), the peak wavelength ( max), and the maximum spectral radiant emittance (W , max) are calculated for the desired temperature by Eqs. 8.15, 8.16, and 8.17, respectively. The graph in Fig. 8.7 is of W /W , max plotted against relative wavelength. Thus, if W for a particular wavelength ( ) is desired, the value of W /W , max corresponding to the appropriate value of / max is selected and multiplied by the value of W , max from Eq. 8.17. Across the top of Fig. 8.7 is a scale which indicates the fraction of the total energy emitted at all wavelengths below that corresponding to the point on the scale. Note that exactly 25 percent of the energy from a blackbody is emitted at wavelengths shorter than max. If it is necessary to determine the amount of power emitted in a spectral band between two wavelengths ( 1 and 2), the wavelengths are converted to relative wavelengths ( 1/ max and 2/ max) and the fractions corresponding to them are selected from the scale at the top of the figure. The total power (WTOT) from Eq. 8.15 times the difference between the two fractions will give the amount of power emitted in the wavelength interval. Example B

For a blackbody at a temperature of 27°C (80.6°F), T is 273  27  300 K, and the total emitted radiation is given by Eq. 8.15 WTOT  5.67  1012(300)4  4.59  102 W/cm2 The wavelength at which W is a maximum is given by Eq. 8.16 max  2897.9 (300)1  9.66 m and the radiant emittance at this wavelength is obtained from Eq. 8.17 W , max  1.288  1015 (300) 5  3.13  103 W cm 2 m1 As an aside, note that this (300 K) is a reasonable value for the ambient temperature and that our result indicates that the earth and most things on it are strongly emitting at a wavelength of 10 m. This is the basis of the “see in the dark” FLIR systems which are sensitive to this spectral region; most such systems use germanium optics, which transmit well in the 8- to 14-m region (which also happens to

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be a good transmission window of the atmosphere). Thus there is no such thing as darkness if you can detect 10-m radiation. Suppose we wish to know the characteristics of this blackbody in the wavelength region between 4 and 5 m. We express these wavelengths in terms of max as 4/9.66  0.414 and 5/9.66  0.518. From Fig. 8.7, the corresponding values of W /W , max are 0.07 and 0.25; these values, multiplied by W , max  3.13  103 W cm2 m1 give us the spectral radiant emittances for these wavelengths At 4 m: W  0.22  103 W cm2 m1 At 5 m: W  0.78  103 W cm2 m1 Using the fraction scale across the top of the chart, we find that about 0.011 of the radiation is emitted below 5 m (rel.  0.518) and about 0.0015 below 4 m. Thus, approximately 1 percent of the total radiation (WTOT), amounting to about 4  104 W/cm2, is emitted in this spectral band. The radiance of the surface will be 4  104/ W ster1 cm2 in this spectral band. If the blackbody is a foot square, with an area of about 1000 cm2, it will radiate about 0.4 W between 4 and 5 m into a hemisphere of 2 ster. Most thermal radiators are not perfect blackbodies. Many are what are called gray-bodies. A gray-body is one which emits radiation in exactly the same spectral distribution as a blackbody at the same temperature, but with reduced intensity. The total emissivity () of a body is the ratio of its total radiant emittance to that of a perfect blackbody at the same temperature. Emissivity is thus a measure of the radiation and absorption efficiency of a body. For a perfect blackbody   1.0, and most laboratory standard blackbodies are within a percent or two of this value. The table of Fig. 8.8 lists the total emissivity of a number of common materials. Note that emissivity varies with both wavelength and with temperature. Radiation incident on a substance can be transmitted, reflected (or scattered), or absorbed. The transmitted, reflected, and absorbed fractions obviously must add up to 1.0. The absorbed fraction is the emissivity. Thus a material with either a high transmission or a high reflection must have a low emissivity. When dealing with gray-bodies, it is necessary to insert the emissivity factor  into the blackbody equations. Planck’s law (Eq. 8.14), the Stefan-Boltzmann law (Eq. 8.15), and the Wien displacement law (Eq. 8.17) should be modified by multiplying the right-hand term by the appropriate value of . For many materials the emissiv-

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Figure 8.8 The total emissivity of a number of materials.

ity is a function of wavelength. This is apparent from the fact that many substances (glass, for example) have a negligible absorption, and consequent low emissivity, at certain wavelengths, while they are almost totally absorbent at other wavelengths. In regions of the spectrum where this occurs, emissivity becomes spectral emissivity ( ) and is treated just as any other spectral function. For many materials, emissivity will decrease as wavelength increases. It should also be noted that most materials show a variation of emissivity with temperature as well as wavelength, and precise work must take this into account. Emissivity usually increases with temperature. Note that not all sources are continuous emitters. Gas discharge lamps at low pressure emit discrete spectral lines; the plot of spectral radiant emittance for such a source is a series of sharp spikes, although there is usually a low-level background continuum. In high-

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237

pressure arcs, the spectral lines broaden and merge into a continuous background with less pronounced spikes. Color temperature

Before leaving the subject of blackbody radiation, the concept of color temperature should be mentioned. The color temperature of a source of light is a colorimetric concept related to the apparent visual color of a source, not its temperature. For a blackbody, the color temperature is equal to the actual temperature in Kelvin. For other sources, the color temperature is the temperature of the blackbody which has the same apparent color as the source. Thus, exceedingly bright or dim sources may have the same color temperature, but radically different radiances or intensities. Color temperature usually runs about 150 K higher than filament temperature. Color temperature is extremely important in colorimetry and in color photography where fidelity of color rendition is important, but is little used in radiometry. 8.9 Photometry Photometry deals with luminous radiation, that is, radiation which the human eye can detect. The basic photometric unit of radiant power is the lumen, which is defined as a luminous flux emitted into a solid angle of one steradian by a point source whose intensity is 1⁄60 of that of 1 cm2 of a blackbody at the solidification temperature of platinum (2042 K). From the preceding section, we know that a blackbody radiates energy throughout the entire electromagnetic spectrum. Chapter 5 indicated that the eye was sensitive to only a small interval of this spectrum and that its response to different wavelengths within this interval varied widely. Thus, if a source of radiation has a spectral power function P( ) (W m1), the visual effect of this radiation is obtained by multiplying it by V( ),* the visual response function which is tabulated in Fig. 5.9. The effective visual power of a source is, therefore, the integral (or summation) of P( ) V( ) d over the appropriate wavelength interval. From the definition of the lumen, it can be determined that one watt of radiant energy at the wavelength of maximum visual sensitivity (0.555 m) is equal to 680 lumens. Therefore, the

*Note that V( ) is customarily the photopic (normal level of illumination and brightness) visual response curve. Under conditions of complete dark adaptation, the visual response for scotopic vision would be used. The conversion constant in Eq. 8.18 becomes 1746 instead of 680.

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Source

Brightness, candles cm-2

Sun (zenith) through atmosphere

1.6 x 105 cd/cm2

Sun (zenith) above atmosphere

2.75 x 105

Sun (horizon) Blue sky

6 x 102 0.8

Dark cloudy sky

4 x 10–3

Night sky

5 x 10–9

Moon

0.25

Exteriors—daylight (typical)

1

Exteriors—night (typical)

10–6

Interiors—daylight (typical)

10–2

Mercury arc—laboratory

10

Mercury arc—high pressure

5 x 105

Xenon arc

1.5 x 104 to 1.5 x 105

Carbon arc

104 to 105

Tungsten—3655 K (melting point)

5.7 x 103

3500 K

4.2 x 103

3000 K

1.3 x 103

Tungsten filament – ordinary lamp – projection lamp Blackbody—2040 K

5 x 102 3 x 103 60.0 (by definition)

—4000 K

2.5 x 104

—6500 K

3 x 105

Fluorescent lamp

0.6

Sodium lamp

6

Flame—candle, kerosene

1

Least perceptible brightness

5 x 10–11

Least perceptible point source

2 x 10–8 cd @ 3 m distance

Star Sirius

1.5 x 106

Atom bomb

108

Lightning

8 x 106

Ruby laser

1014

Metal halide lamp

4 x 104

Figure 8.9 Typical values for the brightness (luminance) of a number of sources.

Radiometry and Photometry

239

luminous flux emitted by a source with a spectral power of P( ) W m1 is given by

冕

F  680 V ( ) P ( ) d lumens

(8.18)

The unit of luminous intensity is called the candle (or “candela”) and is so named because the original standard of intensity was an actual candle. A point source of one candlepower is one which emits one lumen into a solid angle of one steradian. A source of one candle intensity which radiates uniformly in all directions emits 4 lumens. From the definition of the lumen, it is apparent that a 1-cm2 blackbody at 2042 K has an intensity of 60 candles. Illumination, or illuminance, is the luminous flux per unit area incident on a surface. The most widely used unit of illumination is the foot-candle. One footcandle is one lumen incident per square foot. The misleading name footcandle resulted from the fact that it is the illumination produced on a surface one foot away from a source of onecandle intensity. The photometric term illuminance corresponds to irradiance in radiometry. The term brightness, or luminance, corresponds to the term radiance. Brightness is the luminous flux emitted from a surface per unit solid angle per unit of area (projected on a plane normal to the line of sight). There are several commonly used units of brightness. The candle per square centimeter is equal to one lumen emitted per steradian per square centimeter. The lambert is equal to 1/ candles per square centimeter. The foot-lambert is equal to 1/ candles per square foot. The foot-lambert is a convenient unit for illuminating engineering work, since it is the brightness which results from one footcandle of illumination falling on a “perfect” diffusing surface. (Since one lumen is incident on the 1-ft2 area under an illumination of one footcandle, the total flux radiated into a hemisphere of 2 ster. from a perfectly diffuse (lambertian) surface is just one lumen. As pointed out in Sec. 8.4 and Example A, the resulting brightness is 1/ lumen ster1 ft2, not 1/2 lumen ster1 ft2). The brightness of a number of sources is tabulated in Fig. 8.9 and natural illumination and reflectance levels are tabulated in Fig. 8.10. The terminology of photometry has grown through engineering usage, and is thus far from orderly. Special terms have derived from special usages, and many such terms have survived. A tabulation of photometric units is given in Fig. 8.11. Photometric calculations may be carried out exactly as radiometric calculations, using the relationships presented in Secs. 8.2 through 8.6. If lumens are substituted for watts in all the expressions, the computations are straightforward. When the starting and final data must be

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Source

Illumination, footcandles

Direct sunlight

10,000 footcandles

Open shade

1,000

Overcast/dark day

10 to 100

Twilight

0.1 to 1.0

Full moon

0.01 0.0001 0.00001

Starlight Dark night (a) Material

Reflectance

Asphalt

0.05 0.20 0.35 0.40 0.85 0.65 0.70 0.40

Trees, grass Red brick Concrete Snow Aluminum building Glass window wall Parking lot with cars (b)

(a) Illumination levels produced by sources in nature. (b) Reflectance of a number of exteriors. Figure 8.10

expressed in the special terminology of photometry (as opposed to what one might term the rational units of lumens, steradians, and square centimeters), then conversion factors may be necessary for each relationship. A very simple way of avoiding this difficulty is to convert the starting data to lumens, steradians, and square centimeters, complete the calculation, and then convert the results into the desired units. For convenience, the basic relationships are repeated here in both radiometric (left column) and photometric (right column) form: Radiant Intensity: J  P/

Luminous Intensity: I  F/

J is radiant intensity

I is luminous intensity

P is the radiant power emitted into solid angle 

F is the luminous flux emitted into solid angle I

Irradiance: H  J/S2  J

Illumination (illuminance): E  I/S2  I

H is the irradiance incident on a surface a distance S from a point

E is the illumination incident on a surface a distance S from a point

Radiometry and Photometry

241

Figure 8.11 Photometric quantities.

source of intensity J.  is the solid angle subtended by a unit area of the surface from the source.

source of intensity I.  is the solid angle subtended by a unit area of the surface from the source.

H  N sin2  H is the irradiance produced by a diffuse circular source of radiance N at a point from which the source diameter subtends 2.

E  B sin2  E is the illumination produced by a diffuse circular source of brightness (luminance) B at a point from which the source diameter subtends 2.

H  N H is the irradiance produced by a diffuse source of radiance N at a point from which the area of the source subtends the solid angle . H  TN sin2  (H  TN) H is the irradiance at an image formed by an optical system of

E  B E is the illumination produced by a diffuse source of brightness B at a point from which the area of the source subtends the solid angle . E  TB sin2   TB/4(f/#)2 (m  1)2

(E  TB)

s′

冤m  冢 f  1冣 冥

E is the illumination at an image formed by an optical system of trans-

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transmission T whose exit pupil diameter (area) subtends an angle 2 (solid angle ) from the image point when object radiance is N.

mission T whose exit pupil diameter (area) subtends an angle 2 (solid ngle ) from the image point when the object brightness is B.

Radiance: N  P/(A)

Brightness (luminance): B  F/(A)

N is the radiance of a diffuse source of area A which emits radiant power P into a hemisphere of 2 steradians.

B is the brightness of a diffuse source of area A which emits luminous flux F into a hemisphere of 2 steradians.

Example C

It may be instructive to repeat Example A in photometric terms and to indicate at each step in the calculation the conversions to the various photometric units. We will use Fig. 8.5 again; the only change in the starting data will be that the source A will be assumed to have a brightness of 10 lumens ster1 cm2. From Fig. 8.11, we note that the source brightness may also be expressed as 10 candles cm2, as 10 stilb, as 10 lamberts, or as 9290 foot-lamberts. The illumination produced at point B is calculated from Eq. 8.7 (after rewriting it in photometric symbols) H  N sin2  E  B sin2    (10L ster

1

cm ) 2

冢 冣 1  2

 7.85 lumen cm2 Applying the cosine-fourth law, we find the illumination at C EC  EB cos4 45°  7.85  (0.707)4  1.96 lumen cm2 Since there are 929 cm2 per square foot EC  929  1.96  1821 lumens ft2  1821 footcandles

2

Radiometry and Photometry

243

Since the surface BC has a diffuse reflectivity of 70 percent, we can multiply the illumination in footcandles by 0.7 to obtain the brightness in foot-lamberts B  0.7  1821  1275 foot-lamberts Similarly 0.7 times the illumination in lumens cm2 will yield the brightness in lamberts B  0.7  1.96  1.37 lamberts Or we can retain the lumen units, and determine that, with 1.96 lumen cm2 falling on a surface 70 percent reflectivity, 1.37 lumen cm2 will be emitted into a hemisphere, and, following our previous reasoning, compute the brightness as 1.37 B    0.44 lumen ster1 cm2  0.44 candle cm2 The illumination at E is determined from Eq. 8.11 as before H  TN sin2   TN E  TB  0.8  0.44  104  0.35  104 lumen cm2  929  0.35  104  0.032 footcandles 8.10

Illumination Devices

Searchlight

A searchlight is one of the simpler, and at the same time one of the least understood, illuminating devices. It consists of a source of light (usually small) placed at the focal point of a lens or reflector. The image of the source is thus located at infinity. A common misconception is that the beam of light produced is a “collimated parallel bundle” which extends out to infinity with a constant diameter and a constant power density. A little consideration of the matter will

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reveal the fallacy: the rays from any point on the source do indeed form a collimated parallel bundle, etc. However, a geometrical point on any source of finite brightness must emit zero energy, since a point has zero area, and therefore the “collimated bundle” of rays has zero energy. With reference to Fig. 8.12, which shows a source S at the focal point of lens L, the image (S′) will be located at infinity. Since source S subtends an angle  from lens L, the image S′ will also subtend . Now the illumination at a point on the axis will be determined by the brightness of the image and the solid angle subtended by the image. Thus, for points near the lens, the illumination is given by (8.19)

E  TB

which the reader will recognize as Eq. 8.8 rewritten in photometric symbols and with a transmission constant (T) added. B is the brightness of source S (since the brightness of an image equals the brightness of the object) and  is the solid angle subtended by the image. (We have tacitly assumed  to be small.) Now for a point at the lens, it is obvious that the solid angle  subtended by the image S′ is exactly equal to the solid angle subtended by the source S from the lens. Since S′ is at infinity, this angle will not change as we shift our reference point a short distance along the axis away from the lens, and the illumination will remain constant in this region. However, at a distance D  (lens diameter)/, the source image will subtend the same angle as the diameter of the lens, and for points more distant than D, the size of the solid angle subtended by the source of illumination will be limited by the lens diameter. This solid angle will obviously be equal to (area of lens)/d2 and the illumination beyond distance D will fall off with the square of the distance (d) to the lens. Thus, the equations governing the illumination produced by a searchlight are lens diameter D   

(8.20)

for d  D: E  TB  (a constant)

(8.21)

L S TO S' AT INFINITY



 d

ƒ D

Figure 8.12 The optics of a searchlight.

Radiometry and Photometry

TB (lens area) for d  D: E   d2

245

(8.22)

The general technique used here is applicable to almost any illumination problem, and we can restate it in general terms as follows: To determine the illumination at a point, the size and position of the source image, as seen from the point, are calculated. The pupils and windows of the system (again, as seen from the point) are determined. Then the illumination at the point is the product of the system transmission, the source brightness and the solid angle subtended by that area of the source which can be seen from the point through the pupils and windows of the system, multiplied by the cosine of the angle of incidence.

Note that for points (which lie within the beam) beyond the critical distance D, the searchlight acts as if it were a source of a diameter equal to that of the searchlight lens and a brightness TB. As mentioned in Sec. 8.6, this concept is quite useful in evaluating the illumination at an image point; here we find that it occasionally can be applied to points which are not image points. The beam candle power of a searchlight is simply the intensity of the (point) source which would produce the same illumination at a great distance. A point source with an intensity of I candles will emit I lumens per steradian. A one-square-foot area placed d feet from the point source will subtend 1/d 2 steradians from the source, and will thus be illuminated by I/d 2 lumens per square foot (footcandles). We can determine the necessary candle power for I by equating this illumination to that produced by the searchlight according to Eq. 8.22. I TB (lens area) E  2   d d2

(8.23)

and beam candlepower: I  TB (lens area) where I is the beam candle power in lumens per steradian (or candles). Note that the lens area should be specified in the same units as the source brightness. Projection condenser

The second illumination device we shall consider is the projection condenser, which is schematically diagrammed in Fig. 8.13. The purpose of the projector is to produce a bright and evenly illuminated image of the film on the screen. This could be achieved by placing a sheet of dif-

246

Chapter Eight

Figure 8.13 Schematic of a projection condenser system. The condenser

forms an image of the source (lamp filament) in the aperture of the projection lens.

fusing material behind the film and illuminating this diffuser. The resultant image would be dim, because the maximum brightness which the image could achieve would be that of the diffuser, which would be considerably less than that of the lamp. The function of the condenser is to image the source in the pupil of the projection lens so that the lens aperture has the same brightness as the source. When this is done, the screen is illuminated according to Eq. 8.11, where the solid angle is that subtended by the source image (in the projection lens) from the screen. It is apparent that the maximum value for the screen illumination is limited by the size of the projection lens aperture. Therefore, the maximum screen illumination is achieved when the image of the source completely fills the aperture of the lens. This is required for all points within the field of view, and the condenser diameter must be sufficiently large so that it does not vignette, if maximum illumination at the edge of the picture is required. In this regard, note that the ray from the corner of the film to the opposite edge of the lens aperture is the most demanding. The cosine-fourth rule will, of course, reduce the illumination at points off the axis. From the above, one might conclude that with a condenser of sufficient magnification, the image of a very small source could be magnified enough to fill the pupil of the projection lens. The necessary illuminating cone angle is determined by the film gate and its distance to the lens pupil (i.e., to the image of the source). In Chap. 2 we found that the magnification was given by m  h′/h  u/u′. The Abbe sine condition uses m  sin u/sin u′ for systems of reasonable image quality. Since u′ in this case is fixed by the film gate, it is apparent that a large magnification will require a large value of u. The largest value that u can have is 90° with a sine of one; this establishes the limit on the magnification that can be attained. This limit can be expressed as P   1.0 nS

冨 冨

(8.24)

Radiometry and Photometry

247

where P is the aperture of the projection lens,  is the half-field angle of projection, n is the index in which the source is immersed (usually n  1.0 for air), and S is the size of the source. It is impossible for Eq. 8.24 to exceed a value of 1.0; a value of 0.5 is typical of many systems. Note that a value of 0.5 corresponds to a working speed of f/1.0 and that a value of 1.0 would require a working speed of f/0.5. (Eq. 8.24 is analogous to Eq. 9.24 for detector systems.) When the source is irregular in shape, as in “V” filament lamps for example, the solid angle for Eq. 8.11 is determined just as one might expect, by dividing the area of the actual image of the filament by the square of the distance to the screen. Condenser design is discussed in Sec. 13.4. Telescope brightness

The apparent brightness of an image as seen by the eye is a function of the diameter of the pupil of the eye, since it determines the illumination of the retina, in accordance with Eq. 8.11a. When the eye is used with an optical instrument, such as a telescope, the exit pupil of the instrument enters the picture. If the exit pupil is larger than that of the eye, then the apparent brightness of the object seen through the instrument is equal to the brightness of the object (modified by transmission losses and index effects), since the solid angle subtended by the pupil from the retina is unchanged. When the instrument exit pupil is smaller than that of the eye, then the apparent brightness of the object is reduced in proportion to the relative areas of the pupils. The exception to these brightness relationships of object and image occurs when the object is smaller than the diffraction limit of the optical system (e.g., a star). Since this is not an extended source, all the energy in the retinal image is concentrated on a few retinal receptors, and when the magnification and aperture of a telescope are increased so that its exit pupil diameter stays the same, its effective collection area is increased (at the objective) so that more energy is concentrated on the same retinal cells (because the size of the retinal image is the same, being governed by the diffraction limit), resulting in an increase in the apparent brightness of the source. For example, if a high enough power telescope of large aperture is used, stars may be seen in daylight, since their apparent brightness is increased while that of the sky (as an extended object) is not. Integrating sphere

An integrating sphere is often used in the measurement of light and light sources, and also as a uniform lambertian (diffuse) source of light. It is a hollow sphere, coated on the inside with a highly reflec-

248

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tive white diffuse paint. If spot A on the inside of the sphere is illuminated, the light reflected from this spot produces an illumination at some other point B on the inside of the sphere. This illumination varies with the cosines of angles  and  made by the line connecting A and B with the normals to the sphere surface at A and B. Thus the illumination at B varies as cos  cos   D2

(8.25)

where D is the distance from A to B, and this expression, for the inside of a sphere, is a constant. Thus the entire inner surface of the sphere is uniformly illuminated by the light reflected from the illuminated spot. If we cut two small holes in the sphere, one to admit light and the other (in a location not directly illuminated by the first hole) for a light sensor, we have a device which can read the amount of radiation admitted into the sphere without any variation of sensitivity resulting from the direction of the light, the size of the beam, or the position of the beam in the admitting hole. The total radiation emitted by a lamp or other source which is placed inside the sphere can readily be measured. Conversely, if the light sensor is replaced by a source of light, then the other hole becomes an almost perfect, uniform, unpolarized, lambertian source of radiation. Bibliography Note: Titles preceded by an asterisk (*) are out of print. American Institute of Physics Handbook, New York, McGraw-Hill, 1963. Carlson, F., and C. Clark, in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 1, New York, Academic, 1965 (light sources). Eby, J., and R. Levin, in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 7, New York, Academic, 1979 (light sources). *Hackforth, H., Infrared Radiation, New York, McGraw-Hill, 1960. *Hardy, A., and F. Perrin, The Principles of Optics, New York, McGraw-Hill, 1932. *Jamieson, J., et al., Infrared Physics and Engineering, New York, McGraw-Hill, 1963. Kingslake, R., Applied Optics and Optical Design, vol. 2, New York, Academic, 1965 (illumination). Kingslake, R., Optical System Design, San Diego, Academic, 1983.

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249

LaRocca, A., “Artificial Sources,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 10. LaRocca, A., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, D.C., Office of Naval Research, 1985 (sources). Nicodemus, F., “Radiometry,” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 4, New York, Academic, 1967. Norton, P., “Photodetectors,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 15. Snell, J., in W. Driscoll (ed.), Handbook of Optics, New York, McGrawHill, 1978 (radiometry). Suits, G., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985 (sources). Teele, R., in Kingslake (ed.), Applied Optics and Optical Design, vol. 1, New York, 1965 (photometry). *Walsh, J., Photometry, New York, Dover, 1958. Wolfe, W., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (radiometry). Wolfe, W. L., and P. W. Kruse, “Thermal Detectors,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 19. Zalewski, E. F., “Radiometry and Photometry,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 24. Zissis, G., and A. LaRocca, in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978 (sources). Zissis, G., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985. Exercises 1 A point source emits 10 W/ster toward a 4-in-diameter optical system. How much power is collected by the optical system when its distance from the source is (a) 10ft, (b) 1 mi? ANSWER:

(a) 8.73  103 W; (b) 3.13  108 W

2 A 10-candlepower point source illuminates a perfectly diffusing surface which is tilted at 45° to the line of sight to the source. What is the brightness of the surface if it is 10 ft from the source? ANSWER:

0.0707 foot-lamberts, or 2.42  105 candles cm2.

3 A fluorescent lamp 10 in long and 1 in wide illuminates a slit, parallel to the lamp, which is 10 in long and 10 in from the lamp. If the lamp has a brightness of 0.5 candles cm2, what is the illumination (a) at the center of the slit, and (b) at the ends of the slit? (Hint: Divide the lamp into 10 one-inch-square sources.)

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Chapter Eight

ANSWER:

(a) 0.043 lumens cm2, or 40.2 footcandles (b) 0.032 lumens cm2, or 29.9 footcandles

4 A 16-mm projector uses a 2-in f/1.6 projection lens and a lamp with a filament brightness of 3000 candles cm2. If the condenser fills the lens aperture with the filament image, what is the illumination produced on a screen 20 ft from the lens? Assume the transmission of the lens is 95 percent and the transmission of the condenser is 85 percent. ANSWER:

47.9 footcandles, or 5.16  102 phot

5 (a) What is the spectral radiant emittance of a 1000-K blackbody in the region of 2 m wavelength? What is the radiance? (b) If an idealized bandpass filter, transmitting only between 1.95 and 2.05 m, is used, what is the total power falling on a 1-cm2 detector placed 1 m from a 1-cm2 1000-K blackbody? (Use Fig. 8.7.) ANSWER:

(a) emittance 0.89 W cm2 m1; radiance  0.89/  0.283 W cm2

ster

1

1

m

(b) 2.83  106 W 6 Show that, for long projection distances, the maximum lumen output of a projector is given by

ABT F  2 lumens 4 (f/#) where A is the area of the film gate, B the source brightness, T the transmission of the system, and (f/#) is the relative aperture of the projection lens.

Chapter

9 Basic Optical Devices

This chapter will be devoted to the first-order optics of several typical optical systems. The number of systems covered here is, of necessity, limited, and the emphasis is placed on those fundamental principles which are applicable to a broad range of optical systems. The rather straightforward algebraic manipulations and the considerations of image size and position which follow are quite typical of those encountered in the preliminary stages of optical system design. Constructional details of the optical components have been deliberately omitted and are discussed at considerable length in later chapters. Note that the system diagrams in this chapter show the components as simple lenses. These could equally well be mirrors instead of lenses, and typically are fairly complex assemblies of lens elements. 9.1 Telescopes, Afocal Systems The primary function of a telescope is to enlarge the apparent size of a distant object. This is accomplished by presenting to the eye an image which subtends a larger angle (from the eye) than does the object. The magnification, or power, of a telescope is simply the ratio of the angle subtended by the image to the angle subtended by the object.* Nominally, a telescope works with both its object and image located at infinity; it is referred to as an afocal instrument, since it has no focal length. In the following material, a number of basic relationships for telescopes and afocals will be presented, all based on systems with both object and image located at infinity. In practice, small *For large angles, the magnification is the ratio of the tangents of the half-angles. 251

252

Chapter Nine

departures from these infinite conjugates are the rule, but for the most part they may be neglected. However, the reader should be aware that the fact that the object and/or the image are not at infinity will occasionally have a noticeable effect and must then be taken into account. This is usually important only with low-power devices. See also the comments on instrument myopia in Sec. 5.4. There are three major types of telescopes: astronomical (or inverting), terrestrial (or erecting), and Galilean. An astronomical or Keplerian telescope is composed of two positive (i.e., converging) components spaced so that the second focal point of the first component coincides with the first focal point of the second, as shown in Fig. 9.1a.The objective lens (the component nearer the object) forms an inverted image at its focal point; the eyelens then reimages the object at infinity where it may be comfortably viewed by a relaxed eye. Since the internal image is inverted, and the eyelens does not reinvert the image, the view presented to the eye is inverted top to bottom and reversed left to right. In a Galilean, or “Dutch,” telescope, 9.1b, the positive eyelens is replaced by a negative (diverging) eyelens; the spacing is the same, in that the focal points of objective and eyelens coincide. In the Galilean scope, however, the internal image is never actually formed; the object

Figure 9.1 The three basic types of telescope.

Basic Optical Devices

253

for the eyelens is a “virtual” object, no inversion occurs, and the final image presented to the eye is erect and unreversed. Since there is no real image formed in a Galilean telescope, there is no location where cross hairs or a reticle may be inserted. Assuming the components of the telescope to be thin lenses, we can derive several important relationships which apply to all telescopes and afocal systems and which are of great utility. First, it is readily apparent that the length (D) of a simple telescope is equal to the sum of the focal lengths of the objective and eyelens. D  fo  fe

(9.1)

Note that in the Galilean telescope, the spacing is the difference between the absolute values of the focal lengths since fe is negative. The magnification, or magnifying power, of the telescope is the ratio between ue, the angle subtended by the image, and uo, the angle subtended by the object. The size (h) of the internal image formed by the objective will be h  uo fo

(9.2)

and the angle subtended by this image from the first principal point of the eyelens will be h ue   (9.3) fe Combining Eqs. 9.2 and 9.3, we get the magnification fo ue MP     fe uo

(9.4)

and fe  D/(1  MP) fo  MPD/(1  MP) The sign convention here is that a positive magnification indicates an erect image. Thus, if objective and eyelens both have positive focal lengths, MP is negative and the telescope is inverting. The Galilean scope with objective and eyelens of opposite sign produces a positive MP and an erect image. Note that uo can represent the real angular field of view of the telescope and ue the apparent angular field of view, and that Eq. 9.4 defines the relationship between the real and apparent fields for small angles. For large angles, the tangents of the half-field angles should be substituted in this expression.

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From Chap. 6 we recall that the exit pupil of a system is the image (formed by the system) of the entrance pupil. In most telescopes the objective clear aperture is the entrance pupil and the exit pupil is the image of the objective as formed by the eyelens. Using the newtonian expression relating object and image sizes (h′hf/x), and substituting CAe (the exit pupil diameter) and CAo (the entrance pupil diameter) for h′ and h, fe for f, and fo for x, we get fo CA o    MP fe CAe

(9.5)

While the above derivation has assumed the entrance pupil to be at the objective, Eq. 9.5 is valid regardless of the pupil location, as is obvious from the rays sketched in Fig. 9.1. We also can get a simple expression for the eye relief of the Kepler telescope as follows: R  (MP  1) fe /MP The amount of motion of the eyepiece needed to focus the telescope for someone who is nearsighted or farsighted is given by   Df e2 /1000 where  is in millimeters and D is in diopters. Equations 9.4 and 9.5 can be combined to relate the external characteristics (magnifications, fields of view, and pupils) of any afocal system, regardless of its internal construction CA u MP  e  o uo CAe

(9.6)

The erecting telescope, Fig. 9.1c, consists of positive objective and eyelenses with an erecting lens between the two. The erector reimages the image formed by the objective into the focal plane of the eyelens. Since it inverts the image in the process, the final image presented to the eye is erect. This is the form of telescope ordinarily used for observing terrestrial objects, where considerable confusion can result from an inverted image. (An erect image may also be obtained by the use of an erecting prism as discussed in Chap. 4.) The magnification of a terrestrial telescope is simply the magnification that the telescope would have without the erector, multiplied by the linear magnification of the erector system s f MP   o 2 (9.7) fe s1

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where s2 and s1 are the erector conjugates as indicated in Fig. 9.1c. For a scope as shown, fo, fe, and s2 are positive signed quantities and s1 is negative. The resulting MP is thus positive, indicating an erect image. An afocal system is the basis of the laser beam expander. The beam diameter of a laser is enlarged by a factor equal to the MP when the laser beam is sent into the eyepiece end of the telescope. Expansion of the beam reduces the beam divergence. The Galilean form (Fig. 9.1b) is usually preferred because there is no focus (which can cause a breakdown of the air if the laser is powerful) and the optical design characteristics are more favorable. However, the Keplerian form (Fig. 9.1a) is used when a spatial filter (a pinhole at the focus) is necessary. An afocal system can also be used to change the power, focal length, and/or the field of view of another system by inserting it in a space in the system where the light is collimated (i.e., where the object or image is at infinity.) (See Sec. 13.3 and Fig. 13.32.) Note that an afocal system can be used to image objects which are not at an infinite distance. For example, the exit pupil of a telescope is the image of the aperture stop, which is usually at the objective lens. Again, a consideration of the rays diagramed in Fig. 9.1 will indicate that the linear magnification m is the same, regardless of where the object and image are located. The magnification mh′/h is equal to the reciprocal of the angular magnification, MP. Thus, mh′/h1/MP. Note that if the aperture stop is placed at the internal focus, then the afocal system becomes telecentric in both object and image space. 9.2 Field Lenses and Relay Systems In a simple two-element telescope as shown in Fig 9.2a, the field of view is limited by the diameter of the eyelens (as was discussed at greater length in Chap. 6). In the sketch, the solid rays indicate the largest field angle that a bundle may have and still pass through the telescope without vignetting; for the bundle represented by the dashed rays, only the ray through the upper rim of the objective gets through, and vignetting is effectively complete. The function of a field lens is indicated in Fig. 9.2b. If the field lens is placed exactly at the internal image, it has no effect on the power of the telescope, but it bends the ray bundles (which would otherwise miss the eyelens) back toward the axis so that they pass through the eyelens. In this way the field of view may be increased without increasing the diameter of the eyelens. Note that the exit pupil is shifted to the left, closer to the eyelens, by the introduction of a positive field lens. The distance from the vertex of the eyelens to the exit pupil is called the “eye relief” (since the eye must be placed at the pupil to see the full field of view). The necessity for a positive eye relief obviously limits the

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Figure 9.2 The action of the field lens in increasing the field of view.

strength of the field lens that can be used. In practice, field lenses are rarely located exactly at the image plane, but either ahead of or behind the image, so that imperfections in the field lens are out of focus and are not visible. Periscopes and endoscopes

When it is desired to carry an image through a relatively long distance and the available space limits the diameter of the lenses which can be used, a system of relay lenses can be effective. In Fig. 9.3, the objective lens forms its image in field lens A. The image is then relayed to field lens C by lens B which functions like an erector lens. The image is then relayed again by lens D. The power of field lens A is chosen so that it forms an image of the objective at lens B; similarly, field lens C forms an image of lens B in lens D. In this way, the entrance pupil (which, in this example, is at the objective) is imaged at each of the relay lenses in turn and the image of the object is passed through the system without vignetting. The dashed rays emerging from lens A will indicate the large diameters which would otherwise be necessary to cover the same field of view. This type of system is used in periscopes and endoscopes. An optimum arrangement for most optical systems is often the layout with the least total amount of lens power. In a periscope system the minimum power system is simple to design. Given the maximum lens diameter (which is determined by the available space) the image at the field lenses is arranged to fill this diameter, and the clear aperture of the relay lens is filled with the beam. Thus, with reference to Fig. 9.3, the focal length of the objective is set equal to the field lens CA divided

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Figure 9.3 A system of relay lenses.

by the total field of view, and the distance from A to B is the product of the relay lens CA times the f-number of the objective lens. Lenses B, C, D, etc., all have the same focal length, which is half the distance from A to B, and lenses B, C, D, etc., are all working at unit magnification (m  1). This arrangement yields the minimum lens power for the system; this is the best layout for a periscope system. An endoscope is a miniature periscope used to examine the inside of a cavity through a small orifice; they are widely used in medical applications. The size of the optics in a medical endoscope is on the order of 2 or 3 mm in diameter. The equivalent air path is the actual physical path divided by the index of refraction. In an endoscope or periscope, the number of relay stages is determined by the length of the instrument. If the airspaces are filled with glass, the equivalent air path is shortened by a factor equal to the index of the glass, and the number of relay stages is thereby reduced. Rather than simply fill the spaces with rods of glass, the relay lenses are typically made as cemented doublets, with the flint (negative) element made thick enough to fill the space. The outer surface of the flint is made convex so that it functions as the field lens. This is often referred to as a rod-lens endoscope. The reduction in the number of relay components both reduces the cost of the endoscope and improves the image quality (especially by reducing the secondary spectrum and the Petzval field curvature). 9.3 Exit Pupils, the Eye, and Resolution Since almost all telescopes are visual instruments, they must be designed to be compatible with the characteristics of the human eye. In Chap. 5, we saw that the pupil of the eye varied in diameter from 2 mm to about 8 mm, depending on the age of the viewer and the brightness of the scene being viewed. Since the pupil of the eye is, in effect, a stop of a telescopic system, its effect must be considered. For ordinary use, an exit pupil of 3 mm diameter will fill the pupil of the eye and no increase in retinal illumination will be obtained by providing a larger exit pupil. From Eq. 9.5, it is apparent that the maximum effective clear aperture for an ordinary telescope objective is thus limited to

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a diameter of about 3 mm times the magnification. In practice, this is, however, a fairly flexible situation. In surveying instruments exit pupils of 1.0 to 1.5 mm are common, since size and weight are at a premium and resolution is the most desired characteristic. In ordinary binoculars, a 5-mm pupil is usually provided; the added pupil diameter makes it much easier to align the binocular with the eyes. For the same reason, rifle scopes usually have exit pupils ranging in size from 5 to 10 mm. Telescopes and binoculars designed for use at low light levels (such as night glasses) usually have 7- or 8-mm exit pupils in order to obtain the maximum retinal illumination possible when the pupil of the eye is large. In Chap. 5, it was indicated that the resolution of the eye was at best about one minute of arc; Chap. 6 indicated that the angular resolution of a perfect optical system was (5.5/D) seconds of arc when the clear aperture of the system (D) was expressed in inches. One or both of these limitations will govern the effective performance of any telescope, and for the most efficient design of a telescope, both should be taken into account. If two objects which are to be resolved are separated by an angle , after magnification by a telescope their images will be separated by (MP). If (MP) exceeds one minute of arc, the eye will be able to separate the two images; if (MP) is less than one minute, the two objects will not be seen as separate and distinct. Thus, the magnification of a telescope should be chosen so that 1 MP   ( in minutes)  0.0003   ( in radians) (9.8)  where  is the angle to be resolved. For critical work, a magnification value considerably larger than indicated in Eq. 9.8 is often selected in order to minimize the visual fatigue of the viewer. From the opposite point of view, since the resolution of a telescope (in object space) is limited to (5.5/D) seconds, it is apparent that the smallest resolved detail in the image presented to the eye will subtend an angle of (MP) (5.5/D) seconds, and if this angle equals or exceeds one minute, the eye can discern all of the resolved details. Equating this angle to one minute (60 seconds), we find that the maximum “useful” power for a telescope is MP  11D

(9.9)

(when D is in inches). Magnification in excess of this power is termed empty magnification, since it produces no increase in resolution. However, it is not unusual to utilize magnifications two or three times

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this amount to minimize visual effort. The upper limit on effective magnification usually occurs at the point when the diffraction blurring of the image becomes a distraction sufficient to offset the gain in visual facility. Example A

As numerical examples to illustrate the preceding sections, we will determine the necessary powers and spacings to produce a telescope with the following characteristics: a magnification of 4 and a length of 10 in. We will do this in turn for an inverting telescope, a Galilean telescope, and an erecting telescope, and will discuss the effects of arbitrarily limiting the element diameters to 1 in. For a telescope with only two components, it is apparent that Eqs. 9.1 and 9.4 together determine the powers of the objective and eyelens. Thus, we have D  fo  fe  10 in and fo MP    ±4 fe where the sign of the magnification will determine whether the final image is erect () or inverted (). Combining the two expressions and solving for the focal lengths, we get (MP) D fo   (MP)  1 D fe   1  (MP) For the inverting telescope, we simply substitute MP  4 and D  10 in, to find that the required focal length for the objective is 8 in; for the eyelens, it is 2 in. Since the lens diameters are to be 1 in, the exit pupil diameter is 0.25 in (from Eq. 9.5). The position of the exit pupil can be determined by tracing a ray from the center of the objective through the edge of the eyelens or by use of the thin-lens equation (Eq. 2.4), as follows: 1 1 1 1 1 1 1               0.4 s′ f s fe (D) 2 10 s′  2.5 in

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Figure 9.4 The inverting telescope of Example A.

Thus, the eye relief of our simple telescope is 21 2 in. The field of view of this telescope is not clearly defined, since it is determined by vignetting at the eyelens, as consideration of Fig. 9.4 will indicate. The aperture will be 50 percent vignetted at a field angle such that the principal (or chief) ray passes through the rim of the eyelens. Under these conditions dia. eyelens 1 uo      ±0.05 radians 2D 2  10 and the real* field of view totals 0.1 radians, or about 5.7°. This is a poor representation of what the eye will see, however, since the vignetted exit pupil at this angle closely approximates a semicircle 0.25 in in diameter and can thus completely fill a 3-mm eye pupil. The field angle at which no rays get through the telescope is a somewhat more representative value for the field of view. If we visualize the size of uo in Fig. 9.4 as being slowly increased, it is apparent that the ray from the bottom of the objective will be the first to miss the eyelens and the ray from the top of the objective will be the last to be vignetted out. For the example we have chosen, with both lenses 1 in in diameter, it is apparent that the limiting diameter of the internal image will also be 1 in. (For differing lens diameters, it is a simple exercise in proportion to determine the height at which this ray strikes the internal focal plane.) The half field of view for 100 percent vignetting is then the quotient of the semidiameter of the image divided by the objective focal length, or ±0.0625 radians; the total real field is 0.125 radians, or about 7.1°. Thus, for an exit pupil of 0.25 in, the field of view is totally vignetted at 0.125 rad, 50 percent vignetted at 0.1 rad, and unvignetted at 0.075 rad. These three conditions are illustrated in Fig. 9.5, and it is apparent that the “effective” position of the exit pupil shifts inward as the amount of vignetting increases.

*The real field of a telescope is the (angular) field in the object space. The apparent field is the (angular) field in the image (i.e., eye) space.

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Figure 9.5 The vignetting action of the eyelens determines the

field of view in an astronomical telescope.

Ray diagram used to determine field lens power in Example A.

Figure 9.6

Let us now determine the minimum power for a field lens which will completely eliminate the vignetting at a field angle of ±0.0625 rad. From Fig. 9.6, it can be seen that the field lens must bend the rays from the objective so that ray B strikes no higher than the upper rim of the eyelens. The slope of ray B is equal to 1 in (the difference in the heights at which it strikes the objective and the field lens) divided by 8 in (the distance from field lens to objective), or 0.125. After passing through the field lens, we desire the slope to be zero (in this case) as indicated by the dashed ray B′. Using Eq. 2.41, we can solve for the power of the field lens as follows: u′  u  yf 0.0  0.125 (0.5) f f  0.25 1 ff    4 in  We can now determine the new eye relief by tracing a principal ray from the center of the objective through the field and eye lenses.

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yf u′o    0.0625  uf fo u′f  uf  yff  0.0625  0.5 (0.25)  0.0625 ye  yf  u′f fe  0.5  0.0625 (2)  0.375 u′e  u′f  yee  0.0625  0.375 (0.5)  0.25 0.375 y l′e  eye relief  e    1.5 in 0.25 u′e Note that u′e and uo are still related by the magnification, as in Eq. 9.4, where 0.25 u′ MP  e    4 0.0625 uo since the power of the system has not been changed by the introduction of the field lens located exactly at the focal plane. If we desire to locate the field lens slightly out of the focal plane, the general approach would be the same; the distances, ray heights, etc., in the computations would, of course, be modified accordingly. The power of the telescope would be increased if the field lens were placed to the right of the focus, and vice versa. In either case the scope is slightly shortened. For the Galilean version of our telescope, we solve for the component focal lengths by substituting 4 for the magnification in the equations in the second paragraph of Example A and get (4) 10 (MP) D fo      13.33 in 4  1 (MP)  1 D 10 fe      3.33 in 1  (MP) 1  (4) If we assume the aperture stop to be at the objective lens of a Galilean telescope, the exit pupil will be found to be inside the telescope, and we obviously cannot put the viewer’s eye there. Thus in a Galilean scope the aperture stop is not the objective lens but is the pupil of the user’s eye, and the exit pupil is wherever the eye is located. This is usually about 5 mm behind the eyelens. To determine the field of view, we must trace a principal ray through the center of the pupil and passing through the edge of the objective, as indicated in Fig. 9.7. This can be done by assuming some arbitrary value for ue and tracing the ray through, then scaling the ray data by an appropriate constant (as indicated in Chap. 6) to make the ray height at the objective equal to onehalf its clear aperture. To simplify matters, we will assume here that the pupil is coincident with the eyelens; thus, ue is equal to half the objec-

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Figure 9.7 In a Galilean tele-

scope, the field of view is determined by the diameter of the objective lens and the location of the exit pupil, which is usually the pupil of the observer’s eye.

tive diameter divided by the spacing between the lenses, or 0.05 radians in this instance. Since MPue/uo per Eq. 9.4, we can solve for uo0.05/40.0125 radians. The total real field is 0.025 radians (about 1.5°), considerably less than that of the inverting telescope discussed above. Note that the same type of field vignetting considerations as discussed related to the eyelens of the astronomical telescope may be applied to the objective of the Galilean telescope. One must also bear in mind that the direction of the Galilean field of view can be changed by a lateral shift of the viewer’s eye; this is not true for a telescope with a real internal image when the field stop is located at the image. For the erecting telescope example, we will lay out a telescopic rifle sight, with a magnification of 4, a length of 10 in, and a maximum lens diameter of 1 in, as before. For small-caliber (.22) rifles, a 2-in eye relief is acceptable; for heavier guns, eye reliefs of 3 to 5 in are common. Let us assume that we desire an eye relief of 4 in and design the telescope accordingly. The entrance pupil (at the objective) has a diameter of 1 in; by Eq. 9.6, the exit pupil diameter is thus 0.25 in. Again by Eq. 9.6, the apparent field at the eyepiece (ue) is equal to 4uo, where uo is the real field. With reference to Fig. 9.8, it is apparent that ue is limited by the diameter of the eyelens and that for an unvignetted pupil and a 1-in-diameter eyelens, the 4-in eye relief R limits us to an apparent field as follows: 1 ue  4uo  ±  (eyelens dia.  pupil dia.) 2R 1  ±  (1  0.25)  ±0.09375 24 uo  ±0.0234  (±1.3°) To determine the spacing and powers of the components, we note that the length will be L  fo  s1  s2  fe and the magnification will be

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Figure 9.8 Optics of a simple erecting telescope.

fos2 M  fes1 We can combine these expressions and derive equations for s1, s2, and fr in terms of M, L, fo, and fe as follows: fo (L  fo  fe) s1   (Mfe  fo) s1 Mfe Mfe (L  fo  fe) s2     fo (Mfe  fo) Mfe fo (L  fo  fe) s1s2 fr     s1  s2 (Mf e  fo)2 At this point, we are faced with a situation which is very common in the layout stages of optical design. We can elect to proceed algebraically to find an expression for fo and fe which will yield a scope with the desired eye relief R, or we can proceed numerically. In general, for a one-time solution, the numerical approach is usually the better choice, especially if the system under consideration is well understood. If one is likely to design a number of systems of the same type with various parameters, or if one is “exploring” and wishes to locate all possible solutions, the often tedious labor of an algebraic solution may be well repaid. The preceding equations indicate that we have two choices (or degrees of freedom) which we can make, namely fo and fe, and arrive at a 4 scope of 10-in length; we have not, however, included the eye relief in these equations. To resolve this situation numerically, we would now assume some reasonable value for fo, then proceed to test various values of fe, selecting the value of fe which yields the desired value for the eye relief R. Since R is not a critical dimension, a graphic solution (after a few values of fe have been tried), plotting R versus fe would be quite adequate for our purpose. Repeating the process for

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several additional values of fo would then indicate the range of solutions available. To arrive at a solution analytically, we would proceed as follows: a principal ray, starting at the center of the objective lens with some arbitrary slope angle would be ray-traced by thin-lens equations (2.41, 2.42, and 2.43), using the symbolic values for the spacings and lens powers derived from the three equations immediately preceding. The symbolic values for the powers and spacings involved would thus be: fo (L  fo  fe) First airspace  fo  s1  fo   (Mfe  fo) (Mfe  fo )2 1  Erector power r    Mfe fo (L fo  fe) fr Mfe (L  fo  fe) Second airspace  s2  fe  fe   (Mfe  fo) 1 Eyelens power e   fe The expression for the final intercept length of this ray, l′e  ye/u′e is then equated to the eye relief R, and a solution for fe expressed in terms of fo, M, L, and R is extracted. As can be imagined, the procedure is lengthy and the probability of making an error in the derivation is approximately unity for the first few attempts. Careful work and frequent checking are not only advisable, they are mandatory. When the smoke has cleared away, one finds that M 2RL  fo (M 2R  L) fe   M 2 (R  L) fo (M1)2 and that for any chosen value for fo (which is less than L and more than zero), a set of powers and spacings can be obtained which will satisfy our original conditions for power M, length L, and eye relief R. We are now faced, regardless of whether we have arrived via numbers or symbols, with the problem of determining what is a suitable value for fo upon which to base our solution. There are a number of criteria by which to judge the value of a given solution. In general, one desires to minimize the power of the components in any given system; in subsequent chapters, it will become apparent that it is often advisable to minimize one or all of the following: ||, |y|, |y2| (where the symbol |x| indicates the absolute value of x),  is the component power, and y represents the height of either the axial or principal ray on the component, or the element semiclear aperture.

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Avoiding, for a few chapters at least, the rationale behind these desiderata, we shall proceed to indicate the technique. For a number of arbitrarily chosen values of fo, we determine the required values for fr and fe (as well as s1 and s2). Then the values of the component powers o, r, and e (where   1/f ) as well as |||o||r||e| are plotted against fo, resulting in a graph as shown in Fig. 9.9. Note that the minimum || occurs in the region of fo3.5; for want of a better criterion, this is a reasonable choice. To carry the matter a bit further, we can trace an axial ray and a principal ray through each solution. The axial ray has starting data (at the objective) of y0.5 and u0; the principal ray starting data is yp0 and up0.0234375, chosen on the basis of eye relief and eyelens diameter considerations as discussed several paragraphs above. From these ray traces, we can determine the axial ray height y at each lens, y2, and the necessary minimum clear diameter at each lens D2(|y||yp|) to pass the full bundle of rays at the edge of the field. It turns out that under the conditions we have established, the diameter for the objective and eyelens must be 1 in, and the diameter of the erector lens is 0.3125 in for all values of fo. From this information, a graph as shown in Fig. 9.10 can be plotted. The choice of which of the four minima to select must be made on the basis of material which is contained in subsequent chapters. In general, however, a minimum || in this example would reduce the Petzval curvature of field, a minimum |D| would reduce the cost of making the optics, and minimum |D|, |y|, or |y2| would tend to reduce other aberrations, the choice being dependent upon which aberration one most desired to reduce. Assuming that we have chosen fo4, the values of the lens powers and spacings would be determined as follows:

Figure 9.9 Plot of the element

powers for a 10-in-long erecting telescope with 4-in eye relief versus the arbitrarily chosen objective focal length. 0, r, and e are the powers of the objective, erector, and eyelens, respectively.

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Figure 9.10

fo  4 4  4  4  10  4 (4  4  4  10) fe     1.8298 4  4 (4  10)  4 (4  1) (4  1) 4 (10  4  1.8298) s1    1.4737 (4  1.8298  4)  (1.4737)  4  1.8298 s2    2.6965 4  (1.4737)  4  1.8298 fr    0.9529 (4  1.8298  4) 9.4 The Simple Microscope or Magnifier A microscope is an optical system which presents to the eye an enlarged image of a near object. The image is enlarged in the sense that it subtends (from the eye) a greater angle than the object does when viewed at normal viewing distance. The “normal viewing distance” is conventionally considered to be about 10 in; this represents an average value for the distance at which most people see detail most clearly. (Obviously, very young people can see detail in objects a few inches from the eye and mature persons whose visual accommodation is failing may have difficulty focusing on objects several feet away.) The magnification or magnifying power of a microscope is defined as the ratio of the visual angle subtended by the image to the angle subtended by the object at a distance of 10 in from the eye. The simple microscope or magnifying glass consists of a lens with the object located at or within its first focal point. In Fig. 9.11, the object h, a distance s from the magnifier, is imaged at a distance s′ with a

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The simple microscope, or magnifier, forms an erect, virtual image of the object.

Figure 9.11

height h′. As shown, the image is virtual and both s and s′ are negative quantities according to our sign convention. We can readily determine the magnification by using the first-order equations (2.4 and 2.7) as follows. The object and image distance equation 1 1 1      s′ f s is solved for s fs′ s  f  s′ and substituted into the equation for the image height h (f  s′) hs′ h′     f s Now if the eye is located at the lens, the angle subtended by the image is given by h (f  s′) h′ ′     fs′ s′ If the unaided eye were to view the object at a distance of 10 in, the angle subtended would be h   10 in The magnifying power is the ratio between these two angles h (f  s′) ′ (10 in) MP       fs′  h 10 in 10 in     f s′

(9.10)

Thus we find that the magnification produced by a simple microscope depends not only on its focal length but on the focus position chosen. If one adjusts the object distance so that the image is at infinity

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(i.e., s  f and s′  ) and can be viewed with a relaxed eye, then the magnification becomes simply 10 in MP   f

(9.10a)

If the focus is set so that the image appears to be 10 in away (i.e., s′  10 in) then 10 in MP    1 f

(9.10b)

The value of MP given by Eq. 9.10a is conventionally used to express the power of magnifiers, eyepieces, and even compound microscopes. The preceding assumed that the eye was located at the lens. If the image is not located at infinity, the magnifying power will be reduced as the eye is moved away from the lens. If R is the lens-to-eye distance, the magnification becomes 10 (f  s′) MP   f (s′  R)

(9.10c)

Note that if the dimensions are in millimeters, the constant 10 becomes 254. 9.5 The Compound Microscope As illustrated in Fig. 9.12, a compound microscope consists of an objective lens and an eyelens. The objective lens produces a real inverted image (usually enlarged) of the object. The eyelens reimages the object at a comfortable viewing distance and magnifies the image still further. The magnifying power of the system can be determined by substituting the value of the combined focal length of the two components (as given by Eq. 2.45) into Eq. 9.10a fe fo feo   fe  fo  d (fe  fo  d) 10 in 10 in MP     fe fo feo

Figure 9.12 The compound microscope.

(9.11)

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The more conventional way to determine the magnification is to view it as the product of the objective magnification times the eyepiece magnification. With reference to Fig. 9.12, this approach gives s2 10 in MP  Mo  Me    s1 fe

(9.12)

Equations 9.11 and 9.12 yield exactly the same value of magnification, as can be shown by substituting (d  fe) for s2; determining s1 in terms of d, fe, and fo (from Eq. 2.4); and substituting in Eq. 9.12 to get Eq. 9.11. An ordinary laboratory microscope has a tube length of 160 mm. The tube length is the distance from the second (i.e., internal) focal point of the objective to the first focal point of the eyepiece. Thus, by Eq. 2.6, the objective magnification is 160/fo, and rewriting Eq. 9.12 for millimeter measure, we get 160 254 MP    fo fe

(9.13)

Standard microscope optics are usually referred to by their power. Thus, a 16-mm focal length objective has a power of 10 and an 0.5-in focal length eyepiece has a power of 20. The combination of the two would have a magnifying power of 200, or 200 diameters. The resolution of a microscope is limited by both diffraction and the resolution of the eye in the same manner as in a telescope. In the case of the microscope, however, we are interested in the linear resolution rather than angular resolution. By Rayleigh’s criterion, the smallest separation between two object points that will allow them to be resolved is given by Eq. 6.20 0.61 Z  NA where is wavelength and NAn sin U, the numerical aperture of the system. Note that the index n and the slope of the marginal ray U are those at the object. Because of the importance of the numerical aperture in this regard, microscope objectives are usually specified by power and numerical aperture; for example, a 16-mm objective is usually listed as a 10NA 0.25. At a distance of 10 in, the visual resolution of one minute of arc (0.0003 radians) corresponds to a linear resolution of about 0.003 in, or 0.076 mm. When the object is magnified by an optical system, the visual resolution at the object is thus 0.003 in 0.076 mm R     MP MP

(9.14)

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If we now equate the visual resolution R with the diffraction limit Z and solve for the magnification, we find that 0.12 NA MP  

(9.15)

with in millimeters, is the magnifcation at which the diffraction limit and visual limit match. At this power the eye can resolve all the detail present in the image, and setting 0.55 m, any magnification beyond 225 NA is “empty magnification.” However, as with telescopes, magnifications several times this amount are regularly used, as discussed in Sec. 9.3. 9.6 Rangefinders Figure 9.13 is a schematic diagram of a simplified triangulation rangefinder. The eye views the object by two paths; directly through semitransparent mirror M1 and by an offset path via M1 and fully reflecting mirror M2. The angular position of one of the mirrors is adjusted until both images coincide. In the rudimentary instrument shown here, a pointer attached to mirror M2 can be used to read the value of /2; the distance to the object is found from B D  (9.16) tan  where B is the base length of the instrument. In actual rangefinders, a telescope is often combined with the mirror system to increase the

Basic rangefinder optical system. The eye views the object directly through semireflector M1 and also through movable mirror M2. The angular setting of M2 which brings both views into coincidence determines the range. Figure 9.13

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accuracy of the reading, and any one of a number of devices may be used to determine ; the distance is usually read directly from a suitable range scale so that no calculation is necessary. The accuracy of the value of D depends on how accurately  can be measured. For large ratios of D/B, we can write B D  

(9.17)

and differentiating with respect to , we get dD  B2 d

(9.18a)

Substituting B/D into Eq. 9.18a, we find that the error in D due to a setting error of d is D2 dD   d B

(9.18b)

Now d is primarily limited by how well the eye can determine when the two images are in coincidence. This is essentially the vernier acuity of the eye and is about 10 seconds of arc (0.00005 radians). If the magnification of the rangefinder optical system is M, then d is 0.00005/M radians, and the ranging error is 5  105D2 dD  ±  MB

(9.18c)

Thus, the greater the base B and the greater the magnification M, the more accurate the value of the range D. A few of the devices encountered in rangefinders are illustrated in Fig. 9.14. In Fig. 9.14a the end mirrors are replaced by penta-prisms (or “penta”-reflectors), which are constant-deviation devices, bending the line of sight 90° regardless of their orientation. The reason for their use is to remove a source of error, since no change in the relative angular position of the two images is produced by misalignment of the penta-prisms as would be the case with simple 45° mirrors. A double telescope is built into the system to provide magnification; the power of each branch of the telescope must be carefully matched to avoid errors. The coincidence prism is provided to split the field of view into two halves, with a sharply focused dividing line between. In the system as shown, the final image is inverted; an erecting system, either prism or lens, is frequently included. Actual coincidence prisms are usually much more complex than that shown here. A great variety of devices may be utilized to bring the two images into coincidence. Those shown in Fig. 9.14b to d are located between

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Typical rangefinder optical devices. (a) A telescopic rangefinder with coincidence prism and penta-prism end reflectors. (b) Sliding prism used at X to establish coincidence. (c) Pair of sliding prisms used at X. (d) Rotating parallel plate used at X. (e) Counterrotating prisms used at Y to establish coincidence.

Figure 9.14

the objective and eyelens, usually in the region marked X in Fig. 9.14a. The sliding prism of Fig. 9.14b produces a displacement at the image plane which increases with its distance from the image; it is usually an achromatic prism. Figure 9.14c shows two identical prisms with variable spacing, which displace but do not deviate the rays. The rotating block in Fig. 9.14d operates on the same principle. All of the above tend to introduce astigmatism (that is, a difference of focal position in vertically and horizontally aligned images) since they are tilted surfaces in a convergent beam. The counterrotating wedges of Fig. 9.14e can be located in parallel light (region Y in Fig. 9.14a) and thus avoid this difficulty. Note that as one wedge turns clockwise, the other must rotate counterclockwise through exactly the same angle; in this way the vertical deviation is maintained at zero while the horizontal deviation can be varied plus or minus twice the deviation of an individual wedge. These are sometimes called Risley prisms. Another device to produce a variable angle of deviation consists of a fixed plano concave lens and a movable plano convex lens of the same radius with their curved surfaces nested together. When the convex

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lens is located so that its plane surface is parallel to that of the concave lens, the pair produces no angular deviation. However, if the convex lens is rotated (about its center of curvature), the pair effectively becomes a prism and will produce an angular deviation. This device can be executed with spherical surfaces or with cylindrical surfaces. Single-lens reflex (SLR) cameras often incorporate a split-image rangefinder which is based on an entirely different principle than the coincidence rangefinder described above. The viewfinder of an SLR camera consists of the camera objective lens, a field lens, and an eyelens. The field lens is divided into three zones as indicated in Fig. 9.15b. The outer zone functions as a straightforward field lens, redirecting the light at the edge of the field so that it passes through the eyelens. It is made in the form of a plastic Fresnel lens, in which the curved surface of a lens is collapsed in annular zones to a thin plate, as shown in Fig. 9.15a. This has the refracting effect of the lens without its thickness or weight. Such Fresnel lenses are also used as condensers in overhead projectors, as well as in spotlights and signal lamps. The center zone of the SLR field lens is split into two halves. Each half is a wedge prism; the two prisms are oriented in opposite directions. If the image formed by the objective lens is in focus, it is located in the plane of the wedges and the two halves of the image line up with each other. If the image is out of focus, the image through one-half of the split wedge is deviated in one direction; through the other half the deviation is in the other direction and the image is split. The intermediate zone of the field lens has a surface comprised of tiny pyramidal prisms which deviate and break up an out-of-focus image so as to exaggerate the out-of-focus blurring. For many applications the optical rangefinder has been superceded by the laser rangefinder. This is essentially optical radar, where the distance to the target is obtained by measuring the travel time for a pulse of light to reflect from the target and return. In military applications a high-power laser is used; in surveying applications a cooperative target such as a retrodirector (corner-cube prism) is used and a much lower power source is adequate. 9.7 Radiometer and Detector Optics A radiometer is a device for measuring the radiation from a source. In a simple form, it may consist of an objective lens (or mirror) which collects the radiation from the source and images it on the sensitive surface of a detector capable of converting the incident radiation into an electrical signal. A “chopper,” which may be as simple as a miniature fan blade, is usually interposed in front of the detector to provide an alternating signal for the benefit of the electronic circuitry which must amplify and process the detector output.

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Figure 9.15 (a) A Fresnel lens is shown with the equivalent lens from

which it is derived. Each annular zone of the Fresnel lens has the same surface slope as the corresponding zone of the lens. (b) The split-prism rangefinder of a 35-mm SLR camera splits an out-of-focus image in two by means of oppositely oriented wedge prisms in its central zone. If the image is focused on the wedge surface, it is not deviated or split. The area surrounding the split prism is comprised of tiny pyramidal prisms which break up an out-of-focus image and exaggerate its blur. The outer zone is a Fresnel lens acting as a field lens for the camera viewfinder.

The radiometer is widely used for the purpose its name would seem to imply, to measure radiation. However, it is also the basis of many other applications. The receiver in a communications system by which one talks over a beam of light is a sort of radiometer whose output is converted into audible form. The seeker head of an infrared homing air-toair missile (e.g., the Sidewinder) is basically a radiometer whose output is arranged to indicate whether the hot exhaust of an enemy jet is on or off the line of sight. A simple radiometer is sketched in Fig. 9.16. The detector, with a diameter D, is located at the focus of an objective with a focal distance F and a diameter A. The half-field of view of the system is , and since

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Figure 9.16 A simple radiometer

with an objective lens which forms an image of the radiation source directly on the detector cell.

the detector is at the focus of the system, it is apparent that the halffield of view is given by D   (9.19) 2F In the various applications of radiometers, the following characteristics are frequently desirable in the optical system 1. In order to collect a large quantity of power from the source, the diameter A of the system should be as large as possible. 2. In order to increase the signal-to-noise ratio, the size D of the detector should be as small as possible. 3. In order to cover a practical field of view, the field angle  should be of reasonable size (and often, should be as large as possible). The relationship between A and F is, as we have previously noted, a limited one. If the optical system is to be aplanatic* (that is, free of spherical aberration and coma), the second principal surface (or principal “plane”) must be spherical; for this reason, the effective diameter A cannot exceed twice the focal distance F, and the slope of the marginal ray at the image cannot exceed 90°. This limits the numerical aperture of the system to NAn′ sin 90°n′; for systems in air with distant sources the limiting relative aperture becomes f/0.5. There are other limits imposed on the speed of the objective lens; the design of the system may be incapable of whatever resolution is required at large aperture ratios, or physical limitations (or predetermined relationships) may limit the acceptable speed of the objective. We can introduce the effective f/# of the objective by multiplying both sides of Eq. 9.19 by A; setting (f/#)  F/A and rearranging, to get, for systems in air, D (f/#)   (9.20) 2A *The frequent assumption of aplanatic systems in the analysis of radiometric systems is based (1) on the usual need for good image quality and (2) on the fact that the image illumination (irradiance) produced by an aplanatic system cannot be exceeded, so that the assumption provides a limiting case.

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or for systems with the final image in a medium of index n′ A NA  n′ sin u′   (9.21) D Equation 9.21 can also be demonstrated by setting the optical invariant (Eq. 2.54) at the objective (IA/2) equal to the invariant at the image (I1 2Dn′u′) and substituting sin u′ for u′ (in accordance with our requirement for aplanatism). Since the (f/#) cannot be less than 0.5 and sin u′ cannot exceed 1.0, it is apparent that the objective aperture A, half-field angle , and detector size D, are related by

冨

A   1.0 n′D

冨

(9.22)

It should be noted that Eq. 9.22, since it can be derived by way of the optical invariant with no assumptions as to the system between object and detector, is valid for all types of optical systems, including reflecting and refracting objectives with or without field lenses, immersion lenses, light pipes, etc. It is thus quite futile to attempt a design with the left member of Eq. 9.22 larger than unity; in fact, it is sometimes difficult to exceed (efficiently) a value of 0.5 when good imagery is required. This limit is applicable to any optical system, no matter how simple or complex. Equation 9.22 is exactly analogous to Eq. 8.24 for projection or illumination systems. As an example of the application of Eq. 9.22, let us determine the largest field of view possible for a radiometer with a 5-in aperture and a 1-mm (0.04-in) detector. If the detector is in air (n′1.0) we then have, from Eq. 9.22, 5   1.0 or   0.008 radians 0.04 and the absolute maximum total field (0.016 radians) is a little less than one degree (0.01745 radians). An immersion lens at the detector (described below) with an index n′ would increase the maximum field angle to 0.016n′. An immersion lens is a means of increasing the numerical aperture of an optical system by a factor of the index n of the immersion lens, usually without modifying the characteristics of the system. Another way of considering the immersion lens is to think of it as a magnifier which enlarges the apparent size of the detector. The most frequently utilized form of immersion lens is a hemispherical element in optical contact with the detector. In Fig. 9.17, a concentric immersion lens of index n′ has reduced the size of the image to h′/n′. Since the first surface of the immersion lens is concentric with the axial image point, rays directed toward this point are normal to this surface and are not

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9.17 A hemispherical immersion lens concentric with the focus of an optical system reduces the linear size of the image by a factor of its index.

Figure

refracted. For this reason, neither spherical aberration nor axial coma nor axial chromatic is introduced. The optical invariant at the image is h′n′u′, and since u′ is not changed by the immersion lens, it is apparent that as n′ increases, h′ must decrease. In the use of immersion lenses, one must beware of reflection (especially total internal reflection) at the plane surface. Ideally, the detector layer should be deposited directly on the immersion lens. Since immersion lenses are usually resorted to in cases where the angles of incidence are large, total internal reflection can occur if the immersion lens index is high and a low-index layer (air or cement, for example) separates it from the detector. In the application of radiometer-type systems, it is not unusual that one wishes to use an objective of relatively low speed with a small detector and still cover a large field of view. This is readily accomplished by means of a field lens. The field lens is located at (or more frequently, near) the image plane of the objective system and redirects the rays at the edge of the field toward the detector, as indicated in Fig. 9.18. As can be seen from a brief consideration of the figure, the field lens actually images the clear aperture of the objective on the surface of the detector. The optimum arrangement is when the image of the objective aperture is the same size as the detector and s1 A   ()  s2 D This arrangement not only makes a larger field angle possible, but has the advantage of providing an even illumination over a large portion of the detector surface. Most detectors vary in sensitivity from point to point over their surface; with a field lens of focal length given by s1s2 f  s1  s2

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Figure 9.18 Radiometer with field lens to increase the

field of view with a small detector.

the same area of the detector is illuminated regardless of where the source is imaged in the field of view. Field lenses and immersion lenses are frequently combined. Note that the insertion of a field lens in a radiometer does not change the limitations of Eqs. 9.21 and 9.22; it simply permits the use of an objective system with a low numerical aperture by raising the numerical aperture at the detector. Another device to enlarge the field of view of a radiometer with a small detector is the light pipe, or cone channel condenser. In Fig. 9.19, a principal ray from the objective is shown being reflected from the walls of a tapered light pipe. Note that without the light pipe, the ray would completely miss the detector. It is instructive to consider the “unfolded” path of a ray through such a system, as indicated in Fig. 9.20. The actual reflective walls of the light pipe are shown as solid lines; the dashed lines are the images of the walls formed by reflection from each other. This layout is analogous to the prism unfolding technique explained in Chap. 4 as a “tunnel diagram” and allows us to draw the path of a ray through the system as a straight line. Note that ray A in the figure undergoes three reflections before it reaches the detector end of the pipe. Ray B, entering at a greater angle, never does reach the detector, but is turned around and comes back out the large end of the pipe. This is a limit on the effectiveness of the pipe and is analogous to the f/# or numerical aperture limit on ordinary optical systems discussed above in the derivation of Eqs. 9.20 et seq. A light pipe may be constructed as a hollow cone or pyramid with reflective walls in the manner indicated in Figs. 9.19 and 9.20. It is also common to construct them out of a solid piece of transparent optical material. The walls may then be reflective coated or one may rely on total internal reflection if the angles are properly chosen. Note that with a solid light pipe, total internal reflection may occur at the exit face; this can be avoided by “immersing” the detector at the exit end of the pipe. The use of a solid pipe effectively increases its acceptance angle by a factor of the index n of the pipe material; the effect on the

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The action of a reflecting light pipe in increasing the field of view of a radiometer.

Figure 9.19

Figure 9.20 Ray tracing through a light pipe by means of an “unfold-

ed” diagram.

system is exactly analogous to the use of an immersion lens, and the total radiometer system is still governed by Eq. 9.22 as before. Light pipes may be used with field lenses; the most common arrangement is to put a convex spherical surface on the entrance face of a solid pipe. If one were to look into the large end of a pyramidal light pipe, one would see a sort of checkerboard multiple image of the exit face (or detector), as indicated in Fig. 9.20 for a two-dimensional case. The checkerboard is wrapped around a sphere centered on the apex of the pyramidal pipe. This image is, of course, the effective size of the (“magnified”) detector, and the cone of light from the objective, as indicated by rays A and A′ is spread out over this array. This effect is occasionally useful in decorrelating the point-for-point relationship between the detector surface and the objective aperture which is established when a field lens is used. The effect is even more pronounced in a conical pipe.

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The discussion in this section has been devoted to condensing radiation onto a small detector. The tables can be turned. If we replace the detector with a small source of radiation, devices such as field lenses and light pipes can be used to increase the apparent size of the source and to reduce the angle through which it radiates (or vice versa). A common application of the light pipe is in illumination systems, especially where extremely uniform illumination is required and the source is very nonuniform, such as a high-pressure mercury or xenon or metal halide arc lamp. If the light pipe is made with parallel sides (either as a cylinder or with a square or rectangular cross section) as shown in Fig. 9.21, the image of the light source can be focused on one end of the pipe; the other end is then quite uniformly illuminated. As can be seen from the figure, the multiple reflections of the source form a checkerboard array of images which is effectively a new light source, and the illumination across the exit end of the pipe is quite uniform. Of course there is no reason that a tapered pipe cannot be used in this way, and this is occasionally done. Note that the proportions of the light pipe (length, diameter) and the convergence of the imaging beam will determine the number of reflections and the number of reflected source images. 9.8

Fiber Optics

A long, polished cylinder of glass can transmit light from one end to the other without leakage, provided that the light strikes the walls of the cylinder with an angle of incidence greater than the critical angle for total internal reflection. The path of a meridional ray through such a cylinder is shown in Fig. 9.22. The geometric optics of meridional

Figure 9.21 A light pipe can be used to produce very uniform illumination at its exit face

when a light source is focused on the other end. The multiple images produced by reflections from the pipe walls become the illuminating source for the exit face.

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Figure 9.22 Light is transmitted

through a long polished cylinder by means of total internal reflection.

rays through such a device are relatively simple. For a cylinder of length L, the path traveled by the meridional ray has a length given by L Path length   cos U′

(9.23)

and the number of reflections undergone by the ray is path length L No. reflections     tan U′±1 (d/sin U′) d

(9.24)

where U′ is slope of the ray inside the cylinder, d is the cylinder diameter, and L its length. For the light to be transmitted without reflection loss, it is necessary that the angle I exceed the critical angle n2 sin Ic   n1 where n1 is the index of the cylinder and n2 the index of the medium surrounding the cylinder. From this one can determine that the maximum external slope of a meridional ray which is to be totally reflected is 1 sin U   兹苶 n12  苶 n22 (9.25) n0 This “acceptance cone” of a cylinder is often specified as a numerical aperture; by rearranging Eq. 9.25, we get n12  苶 n22 NA  n0 sin U 兹苶

(9.26)

This is the minimum value for the numerical aperture; as indicated below and in Fig. 9.23, skew rays have a larger NA than do meridional rays. Again, with reference to Fig. 9.22, it is apparent that if the meridional ray had entered the cylinder well above or well below the axis, it would have emerged with a slope angle of U. The path of a pair of skew rays is indicated (in an end-on view) in Fig. 9.23. Note that a skew ray is rotated with each reflection and that the amount of

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Figure 9.23 The path of skew

(nonmeridional) rays through a reflecting cylinder is a sort of helix. The amount of rotation a ray undergoes in traversing a given length depends on its entrance position.

rotation depends on the distance of the ray from the meridional plane. Thus, a bundle of parallel rays incident on one end of a cylinder will emerge from the other end as a hollow cone of rays with an apex angle of 2U. If the diameter of the cylinder is small, diffraction effects may diffuse the hollow cone to a great extent. It is also worth noting that since the skew rays strike the surface of the cylinder at a greater angle of incidence than the meridional rays, the numerical aperture for skew rays is larger than that for meridional rays. If the light-transmitting cylinder is bent into a moderate curve, a certain amount of light will leak out the sides of the cylinder. However, the major portion of the light is still trapped inside the cylinder, and a simple curved rod is occasionally a convenient device to pipe light from one location to another. Optical fibers are extremely thin filaments of glass or plastic. Typical diameters for the fibers range from 1 to 2 m to 25 m or more. At these small diameters, glass is quite flexible, and a bundle of optical fibers constitutes a flexible light pipe. Figure 9.24 shows a few of the applications of fiber optics. Figure 9.24a indicates the basic property of an oriented, or “coherent,” bundle of fibers in transmitting an image from one end of the fiber to the other. If the bundle is constrained at both ends so that each fiber occupies the same relative position at each end, then the fiber rope may literally be tied in knots without affecting its image-transmitting properties. Fiber bundles with lengths of many feet are obtainable with surprisingly high transmissions. The limiting resolution (in line pairs per unit length) of a coherent fiber bundle is approximately equal to half the reciprocal of the fiber diameter; by synchronously oscillating or scanning both ends of the fiber, this resolution can be doubled. When the fibers are tightly packed, their surfaces contact each other and leakage of light from one fiber to the next will occur. Moisture, oil, or dirt on the fiber surface can also interfere with total internal reflection. This is prevented by coating or “cladding” each fiber with a thin layer of lower-index

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Figure 9.24 Fiber optics.

glass or plastic. For example, the core glass may have n11.72 and the cladding n21.52, yielding a numerical aperture according to Eq. 9.26 of the order of 0.8. Since the total internal reflection (TIR) occurs at the core-cladding interface, moisture or contact between the outer surfaces does not frustrate the TIR if the cladding is thick enough. Figure 9.24b shows a flexible gastroscope or sigmoidoscope. An objective lens forms an image of the object on one end of a coherent fiber bundle; at the other end the transmitted image is viewed with the aid of an eyepiece or video camera.

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Ordinary photography of a cathode ray tube face is an inefficient process. The phosphor radiates in all directions and a camera lens intercepts only a small portion of the radiated light. A tube face composed of a hermetically fused fiber array (Fig. 9.24c) can transmit all the energy radiated into a cone defined by its NA to a contacted photographic film with negligible loss. Fused fibers are always clad with low-index glass to separate the fibers; frequently an absorbing layer or absorbing fibers are added to prevent contrast reduction by stray light which is emitted at angles larger than the numerical aperture of the fibers. Fiber optics are also available as optical conduit, that is, rigid fused bundles, for efficient transmission of light through labyrinthian paths, as shown in Fig. 9.24d. Flexible plastic fibers with diameters on the order of 0.5 in are used as single fibers in illumination systems. A tapered, coherent, fused-fiber bundle can be used as either a magnifier or minifier (depending on whether the original object is placed at the small or large end of the taper). By twisting a coherent bundle of fibers, either fused or not, an image erector can be made which will carry out the function of the erector prisms described in Chap. 4. These are often found in image-intensifier systems such as those used in night vision goggles. Hollow glass fibers in diameters from 0.5 to 1.0 mm, internally coated, are moderately flexible and have been used to transmit radiation in the 10-m wavelength region. These fibers do a reasonable job of maintaining the gaussian distribution of the laser light. Gradient index fibers

The preceding descriptions have dealt with fibers whose principal function was to transmit power from one end to the other, with little or no concern for any coherence; energy incident on one end of the fiber is effectively homogenized or scrambled and transmitted to the other end. But if the index of the fiber is made high in the center, gradually changing to low at the outside, then the ray paths through the fiber will be curved rather than straight lines. If the index gradient is properly chosen (i.e., approximately a function of the reciprocal of the square of the radial distance from the center of the fiber), the ray paths are sinusoidal as shown in Fig. 9.25. This has two significant effects. Rays originating from a point are brought to a focus periodically along the fiber; thus the fiber is capable of forming an image just as a lens is. This is the basis of the GRIN or SELFOC rod. For example, if the index is given as a function of the radial distance r as n (r)  n0 (1  kr2/2)

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Figure 9.25 In a gradient index rod or fiber (GRIN or SELFOC

rod), light rays travel in sinusoidal paths because the index is high at the center of the rod and lower at the edge. Such a rod can form an image just as a lens does. The rod length shown is the equivalent of two relay lenses and an intermediate-field lens. A short length of rod will act like a single lens element, and a longer length can act like a periscope.

then the focal length of a rod with an axial length of t is 1 ef l   n0 兹苶 k sin (t 兹苶 k) and the back focus is 1 bf l   n0 兹苶 k tan (t 兹苶 k) The “pitch” of the sinusoidal ray path is 2/兹k 苶. Since the focusing effect is continuous along the length of the rod, such a device is the equivalent of the periscope system of relay and field lenses described in Sec. 9.2. A length of rod corresponding to two relay lenses and one intermediate field lens as shown in Fig. 9.25 will thus produce an erect image of an area approximately equal to the rod diameter. A row, or a double row, of such rods is the basis of compact table top (scanning) copy machines. Obviously, a long GRIN rod can function as an endoscope and a short rod (less than a quarter of the length shown in Fig. 9.25) will function like an ordinary lens. This latter is called a Wood lens. The other significant aspect of such an index gradient is that because the light rays travel in sinusoidal paths, they never reach the walls of the fiber and do not depend on reflection at a low-index cladding layer to confine them to the fiber. Also, the optical path (index times distance) is the same for all paths; obviously the axial path is the shortest, but it is at the highest index. This constancy of optical path means that the travel time is the same for all paths over the full numerical aperture; contrast this with the path length given by Eq. 9.23, which varies with the cosine of the ray slope angle. Fibers for communications

Another application for optical fibers is in communication. Using light as an extremely high frequency carrier wave, the data transmission

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rate can be very, very high. Fibers can be made with extremely low absorption (less than 0.1-dB loss per kilometer) so that transmission of information over distances of several miles becomes practical. However, if the lengths of the possible ray paths differ from each other, the elapsed time for light to travel from one end of the fiber to the other will vary from ray to ray. At high data rates, only a small amount of travel time difference is enough to introduce a phase shift sufficient to reduce the signal modulation to a useless level. Again, Eq. 9.23 indicates the path length variation involved. The fibers used for telephone and data transmission are typically single-mode fibers (with core diameters on the order of 10 m) which will not support propagation of a light wave except directly down the length of the fiber. In addition to the variation of path length, another source of trouble results from the fact that in most materials the index varies with wavelength, and thus, even with a constant path length, the optical path would vary with wavelength. Communication fiber materials, in addition to low absorption, are characterized by a very low dispersion in the (narrow) region of the spectrum in which they are used. Silica (SiO2) fibers are made with near zero dispersion at 1.3 m wavelength and very low absorption at 1.55 m. Multilayer cladding can shift the zero dispersion to 1.55 m and flatten it, to make 1.3 to 1.6 m useful. 9.9 Anamorphic Systems An anamorphic optical system is one which has a different power or magnification in one principal meridian than in the other. Such devices usually make use of either cylinder lenses or prisms. With reference to Fig. 9.26c, consider the fan of rays shown in the figure. The left-hand cylindrically surfaced lens is the equivalent of a plane parallel plate for these rays. However, the right-hand lens refracts these rays just as a spherical lens would, because its cylinder axes are at 90° to the left lens. The magnification of this fan of rays is about 0.5 as drawn. If we consider a fan of rays in the other prime meridian, however, the situation is reversed; the lens effect occurs at the left lens and the magnification is about 2.0. Thus the square object figure is imaged as a rectangle four times as wide as it is high. Since the focusing effect of a cylinder varies as the square of the cosine of the angle that a ray fan makes to its power meridian, if both prime meridians are in focus, then all meridians are in focus. Another typical anamorphic system consists of an ordinary spherical objective lens combined with a Galilean telescope composed of cylinder lenses, as indicated in Fig. 9.26. In the upper sketch (a), it is apparent that the cylindrical afocal combination serves to shorten the focal length of the prime lens and thus widen its field of view (for a given film size). In the other meridian (Fig. 9.26b), the cylinder lenses are

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Figure 9.26 Cylindrical anamorphic systems.

equivalent to plane parallel plates of glass and do not affect the focal length or coverage of the prime lens. Thus, the system has a focal length equal to that of the prime lens fp in one direction and a focal length equal to the magnification of the attachment times the prime lens focal length Mfp in the other. In Fig. 9.26 the system is shown as a reversed Galilean telescope with a magnification of less than unity, and Mfp is less than fp. This is the type of system used in many widescreen motion picture processes. The wide angular field is used to compress a large horizontal field of view into a normal film format. The distorted picture which results is expanded to normal proportions by projecting the film through a projection lens equipped with a similar attachment. Note that these attachments are used with ordinary camera and projector equipment. Note that because an anamorphic system has a different equivalent focal length in each meridian, if it is to be focused at a finite distance, it will require a different shift of the lens to focus in each meridian. Thus the prime (spherical) lens must be focused separately from the cylindrical attachment (which is then focused by changing the space between the two components). This type of focusing has the unfortunate effect of changing the anamorphic ratio in a way which makes the face in a close-up appear fatter than it actually is. This is not a popular effect among the acting profession. There are two alternatives to

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this. One is to put a focusing component in front of the system. This is usually a pair of weak spherical elements, one positive and one negative, so that when closely spaced their power is zero; as the spacing between them is increased, their power becomes positive and the system is focused on a close distance. This is, in effect, a collimator for the object. The other alternative is called a Stokes lens, which consists of a pair of weak cylinders of equal but opposite powers, placed between the two components of the afocal cylindrical attachment, with their axes tilted at 45° to the axes of the attachment. When the two Stokes cylinders are counterrotated, both meridians of the system are focused at the tame time. A Bravais system is the finite conjugate analog of an afocal power changer. Figure 9.27 shows the principle of a Bravais system inserted into the image space of an optical system for the purpose of increasing the size of the image without changing the image location. The component powers of this type of system can be determined from Eqs. 2.49 and 2.50 by setting the object to image distance T (the “track length”) equal to zero. (Note that the arrangement shown here is usually much more satisfactory than that with the component powers reversed, which reduces the image size.) If a Bravais system is made with cylindrical optics, the image can be enlarged in one meridian and not in the other. This is of course an anamorphic system and has been successfully used for motion picture work. The value of such a “rear” anamorphic attachment is that its size is much less than that of the equivalent afocal attachment placed in front of the lens; this feature is especially important for use with long-focus zoom lenses, where the necessary size for a “front” anamorph can be overwhelming. In addition, there is no focus problem and no “fat” problem. Cylinder lenses are also used to produce line images where a narrow slit of light is required. The image of a small light source formed by a cylinder lens is a line of light parallel to the axes of the cylindrical surfaces of the lens. The width of the line is equal to the image height

Figure 9.27 Bravais system.

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given by the first-order optical equations; the length of the line is limited by the length of the lens, or as shown in Fig. 9.26c, it may be controlled by another cylindrical lens oriented at 90° to the first. A prism may also be used to produce an anamorphic effect. In Sec. 9.1 (Eqs. 9.5 and 9.6), we saw that the magnification of an afocal optical system was given by the ratio of the diameters of its entrance and exit pupils. A refracting prism, used at other than minimum deviation, has different-sized exit and entrance beams and thus produces a magnification in the meridian in which it produces a deviation. Thus a single prism may be used as an anamorphic system. To eliminate the angular deviation, two prisms, arranged so that their deviations cancel and their magnifications combine, are usually used. Figure 9.28

CA

CA

CA

CA

LASER DIODE

ASPHERIC COLLIMATOR LENS

WEAK CYLINDER LENS

Figure 9.28 The anamorphic action of refracting prisms.

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illustrates the action of a single prism and also shows a compound anamorphic attachment made up of two prisms. Since the anamorphic “magnification” of a prism is a function of the angle at which the beam enters the prism, a variable-power anamorphic can be made by simultaneously rotating both prisms in such a way that their deviations always cancel. Prism anamorphic systems are “in focus” and free of axial astigmatism only when used in parallel (collimated) light. Unlike cylindrical systems, they cannot be focused by changing the space between elements. For this reason, prism anamorphics are frequently preceded by a focusable pair of spherical elements which collimate the light from the object. For use in systems which are not monochromatic, the prisms must be achromatized (as discussed in Sec. 4.5). Prism anamorphs have been used to project wide-screen (anamorphosed) movies; in this application, each achromatic prism component typically consisted of two or three prism elements. The useful field of such a device is rather small; being completely unsymmetric, it has all (both odd and even) orders of aberrations, including some unusual kinds of lateral color and distortion. A laser diode is a useful light source, but it has two properties which ordinarily are a handicap: The output beam is not circular in cross section, but elliptical, and the source itself has a small but significant amount of astigmatism so that instead of appearing as a simple point, it appears as a point in different longitudinal locations for each meridian. The lower sketch in Fig. 9.28 shows a laser diode collimator, consisting of an aspheric surfaced collimator singlet, a weak cylindrical lens to cancel out the source astigmatism, and an anamorphic prism pair to convert the elliptical beam to one with a circular cross section. Note that the nearly monochromatic character of the output radiation makes achromatism unnecessary. 9.10

Variable-Power (Zoom) Systems

The simplest variable-power system is a lens working at unit power. If the lens is shifted toward the object, the image will become larger and will move further from the object. If the lens is moved away from the object, the image will become smaller and will again move away from the object. Thus one may find any number of conjugate pairs for which the object-to-image distance is the same but which have magnifications which are reciprocals of each other. Figure 9.29 indicates the relationships involved in this arrangement. The algebraic expressions shown can be derived readily by manipulation of the thin-lens equation (Eq. 2.4).

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Figure 9.29 The basic unit power zoom lens. The graph indicates

the shift of the image as the lens is moved to change the magnification.

The applicability of this particular zoom system is limited, since the commercial demand for variable-power systems at unit magnification is quite modest. However, by combining the moving element with one or two additional elements (usually of opposite sign), the zoom system can be made to operate at any desired set of conjugates. Several such arrangements are shown in Fig. 9.30. Note that in each system the moving lens passes through a point at which it works at unit magnification. By adding either a positive or negative eyelens or by simply adjusting the power of the last lens of the system, as indicated in the lower sketch, a telescope or afocal attachment may be made. A system which is in focus only at two different magnifications is called a bang-bang zoom. It can be quite useful if what is wanted is a system with just two magnifications (and a continuous “zooming” action is not necessary). Since a bang-bang system is much easier and cheaper to design and build than a continuously in-focus zoom, it is often well worth considering whether a true zoom is really needed in a

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Figure 9.30 Zoom systems based

on the unit power principle.

given application, or whether a simple choice of two magnifications, focal lengths, or powers would be sufficient. All variable-power systems with a single moving component have the same characteristic relationship between image shift and magnification (or focal length). Thus for an uncompensated “single-lens” zoom system, there can be at most two magnifications at which the image is in exact focus. At all other powers, the image will be defocused. This situation can be alleviated in two ways. A “mechanically compensated” zoom system is one in which the defocusing is eliminated by introducing a compensating shift of one of the other elements of the system, as exemplified by Fig. 9.31. Since the motion of the compensating element is nonlinear, it is usually effected by a cam arrangement, hence the name “mechanically compensated.” In a zoom system, the motion of the elements will, of course, cause the ray heights, angles, etc. to change. It is apparent that the chromatic contributions of a single element (which are proportional to y2/V and yyp/V for axial and lateral chromatic, respectively) will vary accordingly. Thus, in order to achieve a fully achromatic system through the zoom, each component must be individually achromatized. However, since a small amount of chromatic often can be tolerated, singlet components are not uncommon. The formulas for a thin-lens layout of this type of system are shown in Fig. 9.31 and can be derived by manipulation of the first-order expressions of Chap. 2. To use the formulas, one may arbitrarily select a value for A, the power of the first element, then determine B, C, and the spacings for the “minimum shift” setting. To find the spacings for other positions of the moving lens, choose a value for one space and solve for the position of the compensating element to maintain the final focus at the same distance from the fixed element.

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Figure 9.31 Mechanically compensated zoom system.

Given: , power (1/efl) of a system at “minimum shift” M, ratio of power at S10 to power at S1(R  1)/RA R  兹苶 M Choose: A, power of the first element. May be an arbitrary choice, or set A  (R  1)/R(S1  S2) to control the length, (S1  S2), at “minimum shift” Then: B  A(R  1)  (1  M)/R(S1  S2) C  (A  )R(R  1)/(3R  1) to get  at the “minimum shift” position “minimum shift” occurs at S1  (R  1)/A(R  1)  RS2  R(S1  S2)/(1  R) S2  (R  1)/AR(R  1)  S1/R  (S1  S2)/(1  R) l′  (3R  1)/R(R  1) (3R  1) (R  1) S1  S2  l′     AR R(R  1) Motion of lens C is computed to hold the distance from lens A to the focal point at a constant value as lens B is moved.

It should be apparent that despite the use of three components in the preceding discussion, only two components are necessary to make a mechanically compensated zoom lens. Given any two components, if we change the space between them, Eqs. 2.44 and 2.45 indicate that the effective focal length will be changed. Of course, the back focal length will also change (according to Eq. 2.46), and the entire system will have to be shifted to maintain the focus. It usually turns out to be advantageous if one component is positive and the other negative. There are thus two possible arrangements, depending on which power comes first, and one’s choice can be based on size and focal-length considerations. Many of the newer 35-mm camera zoom lenses are of this type. Many of the newer zoom lens designs have more than two moving components. The extra motion may be used to improve the image quality through the zoom or to stabilize the image quality when the lens is focused at a near distance.

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The other technique for reducing the focus shift in a variable-power system is called optical compensation. If two (or more) alternate lenses are linked and moved together with respect to the lenses between them, the powers and spaces can be so chosen that there are more than two magnifications at which the image is in exact focus. Two systems of this type are shown in Fig. 9.32. In the upper sketch, the first and third elements are linked and move to produce the varifocal effect. The second element, the other elements, and the film plane are all held in a fixed relationship with each other. The image motion produced by this type of system is a cubic curve, as shown in the upper graph. It is thus possible to arrange the powers and spaces so that the image is in exact focus for three positions in the zoom. The defocusing between these points is greatly reduced in comparison with the simpler systems described above, and if the range of powers is modest and the focal length of the system is short, a nonlinear compensating motion of one of the elements is not necessary. In the second system of Fig. 9.32, the motion of the image is described by a still-higher-order curve, and four points of exact compensation are possible; the residual image shift is about one-twentieth of the shift of the upper system. It turns out that the maximum number of points of exact compensation is equal to the number of variable airspaces. (Note that in Fig. 9.30 this number is 2, and the image motion is parabolic with two possible points of compensation.) Originally it was thought that the fabrication of a mechanically compensated zoom lens would be almost impossibly difficult, requiring an unattainable level of precision, which could not be maintained as the cams, etc., wore with use. This turned out to be an incorrect assumption, and mechanically compensated zoom systems are widely used for almost all applications. Optical compensation is rare for several

Figure 9.32 Optically compensated zoom systems. The upper system

has three “active” components and three points of compensation as indicated in the upper graph. The lower system has four “active” components and four compensation points.

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reasons. The requirements of the power and space layout to achieve optical compensation are extremely stringent and restrict the lens designer’s ability to maintain the correction of the lens system throughout the zoom range. In addition, the size of the optically compensated system is significantly larger than the equivalent mechanically compensated system. Despite the fact that the optically compensated lens with its simple and undemanding mechanics is less expensive to fabricate, provided size is not a problem, the optically compensated zoom is effectively obsolete. In zoom systems the focal lengths of a stationary first element and of the elements following the last moving lens may be changed at will, provided the relationship between the focal points of the elements is maintained. Such changes modify the focal length (or power) of the overall system and, in the case of the following elements, the amount of image shift as well. However, since a change in object position will shift the focus point of the first element with respect to the other elements, a zoom system is sensitive to object position. In order to maintain precise compensation, most zoom lenses are focused by moving an element of the first component with respect to the rest to offset this effect. As with the anamorphic systems discussed in Sec. 9.9, the leading component serves to collimate the light from the object. 9.11 The Diffractive Surface The diffractive surface (or “kinoform” or “binary surface”) as used in imaging optics is discussed at some length in connection with the design of telescope objectives in Chap. 12. In this section we are concerned not with the kinoform’s Fresnel surface modulo 2 but with those surfaces which operate on the basis of diffraction in order to introduce a controlled diffusion or to produce a message or a pattern from a simple laser beam. Often these surfaces are simple two-, four-, or eight-level patterns with randomized surface elevations. These devices are made feasible by the recent advances in fabrication technology which make it possible to produce the microscopic wavelength-sized surface details required to produce these effects. To those who think in terms of the phasefront or wavefront, the form of such a device is derived by describing the phasefront which will produce the desired effect and then determining the surface contour which will impose this phasefront on the input beam. However, for those who think geometrically, this is a less than satisfying explanation of how such a surface functions. The following are not elegant depictions, but they do serve the purpose of taking some of the mystery out of such devices.

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The diffusing surface can be visualized as a surface randomly covered with microscopic lenses of a scale on the order of several wavelengths, either concave or convex, whose ratio of diameter to focal length equals the diffusion angle. Such diffusers are commercially available in diffusions of 1 2°, 1°, etc. They can be useful in a number of applications, such as where one desires to destroy the spatial coherence in a laser system in order to eliminate interference patterns. The surface lens concept is not necessary; the same result can be produced by a stepped surface which locally alters the phase of the wavefront. The pattern-generating surface is a little more difficult. Visualize a surface covered with weak prisms, each of which directs its portion of the incoming laser beam in a direction which will form a specific part of the desired pattern. When such a surface is produced on a microscopic wavelength scale, there are many, many tiny prisms in the area covered by the beam, and when the beam is translated across the surface, there are always enough prisms within the beam to produce the pattern. The bigger the beam diameter, the more prisms will be involved, and the better the definition of the pattern will be. There is an inherent “speckle” produced in this process which shows up as a random pattern of dots in the final image. Again, the effect can be produced by stepped surfaces which alter the wavefront diffractively to produce the desired patterns. Bibliography Note: Titles preceded by an asterisk (*) are out of print. Allard, F. (ed.), Fiber Optics Handbook, New York, McGraw-Hill, 1990. Benford, J., and H. Rosenberger, “Microscopes” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 4, New York, Academic, 1967. Bergstein, L., and L. Motz, J. Opt. Soc. Am., vol. 52, April 1962, pp. 363–388 (zoom lenses). Brown, T. G., “Optical Fibers and Fiber-Optic Communication,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 10. Habell, K., and A. Cox, Engineering Optics, Pitman, 1948. Inoue, S., and R. Oldenboug, “Microscopes,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 17. *Jacobs, D., Fundamentals of Optical Engineering, New York, McGraw-Hill, 1943. Johnson, R. B., “Lenses,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 1. Keck, D., and R. Love, “Fiber Optics for Communications” in Kingslake, R., and B. Thompson (eds.), Applied Optics and Optical Engineering, vol. 6, New York, Academic, 1980.

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Kingslake, R., Optics in Photography, SPIE Press, 1992. Kingslake, R., Optical System Design, San Diego, Academic, 1983. Kingslake, R., “The Development of the Zoom Lens,” J. Soc. Motion Picture and Television Engrs., vol. 69, August 1960, pp. 534–544. Legault, R., in Wolfe and Zissis, The Infrared Handbook, Washington, Office of Naval Research, 1985 (reticles). Melzer, J., and K. Moffitt, Head Mounted Displays, New York, McGraw-Hill, 1997. Moore, D. T., “Gradient Index Optics,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 9. Patrick, F., “Military Optical Instruments” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 5, New York, Academic, 1969. Siegmund, W., “Fiber Optics” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 4, New York, Academic, 1967. Siegmund, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978 (fiber optics). Smith, W. J., Practical Optical System Layout, New York, McGrawHill, 1997. Smith, W. J., “Techniques of First-Order Layout,” in Handbook of Optics, vol. 1, New York, NcGraw-Hill, 1995, Chap. 32. Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985. *Strong, J., Concepts of Classical Optics, New York, Freeman, 1958. Wetherell, W. B., “Afocal Systems,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 2. Wetherell, W. B., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 10, San Diego, Academic, 1987 (afocal systems). Wolfe, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985 (scanners). Exercises 1 (a) What focal lenghts are required for the eyelens and objective of a 20  astronomical telescope which is 10 in long? (b) What is the eye relief? (c) What is the minimum objective diameter if the diffraction limit of resolution is to match the resolution of the eye? (d) What is the maximum real field of the telescope if the diameter of the eye lens is 0.5 in? ANSWER:

(a) 10 in/21; 200 in/21 (b) 1 2 in (c) 1.83 in (d) ±0.0296 radians

2 It is desired to add an afocal attachment in front of a 10-in f/10 camera lens to convert it to a 5-in focal length. (a) What element powers are necessary for

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a 3-in length reverse Galilean telescope to accomplish this? (b) What diameter must the outer element have if vignetting is not to exceed 50 percent for an object field of ±60°? Sketch the system. Is this a reasonable diameter? ANSWER:

(a) f0  3 in; fe  6 in (b) 31 2 in

3 A microscope is required to work at a distance of 3 in from the object to the objective. If the objective and eyepiece both have 2-in focal lengths, what is the length of the microscope and what is its power? ANSWER:

Length8 in; power10

4 What is the magnification produced by a telescope made up of a 5-in focal length objective and a 5-in focal length eyepiece (and thus nominally of unit power) when it is set at minus 2 diopters (i.e., the image of an infinitely distant object is 20 in from the eyelens)? ANSWER:

1.25 (with eye at eyelens) or 0.8 (with eye at exit pupil)

5 What base length must a rangefinder have to measure a range of 2000 m to an accuracy of ±0.5 percent if it incorporates a 20-power telescope? ANSWER:

1m

6 Determine the focal length, diameter, and position (relative to the detector) for a radiometer field lens. The objective is a 5-in diameter f/4 paraboloid and the detector is 0.2-in square. The field to be covered is ±0.02 radians. ANSWER:

f  0.77 in; diameter  0.8 in minimum; s2  0.8 in

7 The entrance opening of a tapered hollow light pipe is twice the exit opening. What is the largest angle a ray through the center of the entrance opening can make with the axis and still emerge from the small end of the pipe? ANSWER:

30° (for a long pipe) and 90° (for a short pipe)

8 A hemicylindrical rod (plano-convex) with a cylindrical radius of 2.5 mm, which is 20 mm long, is located 50 mm from a 1-mm-square source of light. At the “focus,” what is the size of the illuminated area? (Assume the rod index is 1.5) ANSWER:

0.111 mm  22.222 mm

9 Determine the element powers and spacings for a zoom lens of 10-in vertex length (s1s210 in) with a zoom ratio of 4 which is to have a 10-in focal length at the “minimum shift” position. Plot the compensating motion of element C against the focal length of the lens as the element B is moved. Use Fig. 9.31. ANSWER:

M4; powers: 0.05, 0.15, 0.18; spacings: 6.67 in, 3.33 in back focus: 8.33 in M1 4; powers: 0.1, 0.15, 0; spacings: 3.33 in, 6.67 in; back focus: 6.67 in

Chapter

10 Optical Computation

10.1 Introduction The analysis of an optical system requires a great deal of numerical computation, devoted, for the most part, to the determination of the exact paths taken by light rays as they pass through the system. As previously mentioned, a ray may be traced by the application of Snell’s law at each surface. There have been a great variety of formulations devised for raytracing. Early formulas were designed for use with logarithms, and then formulas which were optimized for use with mechanical desk calculators were widely used (the trigonometric equations in Chap. 2 are of this type). Today the most widely used tool for raytracing is the electronic computer, and the equations presented in this chapter are designed for this usage, although they can of course be used with a desk or electronic calculator. These equations do not require that a special computation be carried out for long radii or plane surfaces. They are further characterized by the fact that the quantities involved in them are “bounded,” i.e., the maximum size of each term of an equation is readily predicted in terms of the size of the optical system. The latter sections of the chapter will present detailed directions for computing the numerical values of the aberrations discussed in Chap. 3 and also equations for determining the third-order aberration contributions of surfaces and of thin lenses. The precision required of an optical calculation is at least six places, obviously depending on the scale of the optical system and the application to which it is put. Trigonometric functions should be carried to at least six places after the decimal; this corresponds to an error of about one-fifth second of arc and is adequate for all but very demanding 301

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applications. For moderate-sized systems, linear dimensions are carried to five- or six-figure accuracy. Very large diffraction-limited systems will, of course, require greater precision throughout. For most calculations, the modern computer (or PC) in single-precision mode is adequate. Double precision is usually used for diffraction and optical path-length calculations. The time required for an optical computation will obviously depend on the technique and equipment utilized. Tracing a meridional ray (or computing the third-order aberration) through a single surface on a desk calculator is a matter of a minute or so for an experienced operator with a well-thought-out scheme of computation. A skew raytrace is about an order of magnitude more time consuming. The time required on an electronic computer is a matter of fractions of a second on older machines and microseconds on the more powerful machines. The task presented by raytracing is this: given an optical system defined by its radii, thicknesses, and indices, and a ray defined by its direction and its spatial location, to find the direction and spatial location of the ray after it passes through the system. Each set of raytracing equations will be presented in four operational sections. First, the “opening” equations, which start the ray into the system; second, the “refraction” equations, which determine the ray direction after passing through a surface; third, the “transfer” equations, which carry the computation to the next surface; and fourth, the “closing” equations, which permit the determination of the final intercept length or height. The refraction and transfer equations are used iteratively, i.e., they are repeated for each surface of the system. The opening and closing equations are used only at the start and finish of the computation. The reader may note that the coordinate system has been changed from that used in the first and second editions of this book, wherein the optical axis was the x axis. The optical axis in this edition is the z axis. 10.2

Paraxial Rays

Although the paraxial raytracing equations were presented in Chap. 2, they are repeated here (in slightly modified form) for completeness. Opening: 1. Given y and u at the first surface or 2.

y  lu

(10.1a)

or 3.

y  hsu

(10.1b)

cy(n′n) nu u′     n′ n′

(10.1c)

Refraction:

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303

Transfer to the next surface: yj  1  yj  tu′j

(10.1d)

uj  1  u′j

(10.1e)

Closing: yk l′k   u′k

(10.1f)

h′  yk  s′ku′k

(10.1g)

or

The symbols have the following meanings: the height at which the ray strikes the surface; positive above the axis, negative below.

y u

the slope of the ray before refraction.

u′

the slope of the ray after refraction; ray slopes are positive if the ray must be moved clockwise to reach the axis.

h

the height in the object plane at which the ray originates; sign convention same as y.

h′

the height at which the ray intersects the image plane.

l

the distance from the first surface of the system to the axial intercept of the ray; negative if intercept point is to the left of the surface.

l′

the distance from the last surface to the final axial intercept of the ray; positive if the intercept is to the right of the last surface.

s

the distance from the first surface to the object plane; negative if the object plane is to the left of the surface.

s′

the distance from the last surface to the image plane; positive if the image plane is to the right of the surface.

c

the curvature (reciprocal radius) of the surface, equal to 1/R; positive if the center of curvature is to the right of the surface.

n

the index of refraction preceding the surface.

n′

the index of refraction following the surface.

t

the vertex spacing between surfaces j and j1, positive if surface j1 is to the right of surface j.

n and n′

are positive when the ray travels from left to right, negative when the ray travels from right to left (as it does following a single reflection).

k

subscript indicating the last surface of the system.

The physical meanings of the symbols are indicated in Fig. 10.1.

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Figure 10.1 Diagrams to illustrate the symbols used in the paraxial ray-

tracing equations (10.1a through 10.1g).

10.3

Meridional Rays

Meridional rays are those rays which are coplanar with the optical axis of the system. The plane in which both ray and axis lie is called the meridional plane, and, in an axially symmetrical system, a meridional ray remains in this plane as it passes through the system. The two-dimensional nature of the meridional ray makes it relatively easy to trace. Although a great amount of information about an optical system can be obtained by tracing a few meridional rays plus a Coddington trace or two (Sec. 10.6), given the speed of the modern computer, meridional rays are usually traced as a special case of a skew or general raytrace. However, if rays are to be traced with an electronic pocket calculator, then meridional rays are the obvious choice. The formulas in this section are designed to take advantage of the trigonometric capabilities of this type of calculator. Opening: 1. Given Q and sin U at the first surface.

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305

or 2.

Q  L sin U

(10.2a)

or 3.

Q  H cos U  s sin U

(10.2b)

sin I  Qc  sin U

(10.2c)

n sin I sin I′   n′

(10.2d)

U′  UI  I′

(10.2e)

Q (cos U′  cos I′) Q′   (cos U  cos I)

(10.2f)

Qj  1  Q′j  t sin U′j

(10.2g)

Uj  1  U′j

(10.2h)

Q′k L′k   sin U′k

(10.2i)

Q′k  s′k sin U′k H′   cos U′k

(10.2j)

Refraction:

Transfer:

Closing:

or

Miscellaneous: sin (IU) Q [1  cos (IU) ] Q′[1  cos (IU)] y       (cos U  cos I) c (cos U′  cos I′)

(10.2k)

Q sin (IU) 1cos (IU)  z    (cos U  cos I) c

(10.2l)

t  z1  z2 D1 to 2   cos U′1

(10.2m)

The symbols used are, for the most part, the same as those defined in Sec. 10.2, capitalized to differentiate them from the lowercase paraxial symbols. Symbols new to this section are Q

the distance from the vertex of the surface to the incident ray, perpendicular to the ray; positive if upward.

Q′

the distance from the surface vertex to the refracted ray, perpendicular to the ray.

I

the angle of incidence at the surface; positive if the ray must be rotated clockwise to reach the surface normal (i.e., the radius).

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Figure 10.2 Diagram illustrating the symbols used in the meridional raytracing equations.

I′

the angle of refraction.

z

the longitudinal coordinate (abscissa) of the intersection of the ray with the surface; positive if the intersection is to the right of the vertex.

D1 to 2

the distance along the ray between surface 1 and surface 2.

The physical meanings of the symbols are indicated in Fig. 10.2. Example A

As a numerical example, we will trace a paraxial and a meridional ray through the marginal zone of an equiconvex lens with radii of 50 mm, a thickness of 15 mm, and an index of 1.50. We will trace rays originating at an axial point 200 mm to the left of the first surface and determine the axial intersections for both rays after passing through the lens. We will also determine the height at which the marginal (meridional) ray intersects the paraxial focal plane. Assuming the lens to have an aperture of 40 mm, we will use a value of 0.1 for both the paraxial u and the meridional sin U, so that the ray passes through the lens about 20 mm from the axis. The following tabulation indicates both the calculation and a convenient way of arranging the raytrace data. Graphical raytracing (see Fig. 10.3). Meridional rays can be traced using only a scale, straightedge, and compass. The ray is drawn to the surface, and the normal to the surface is erected at the ray-surface intersection. Two circles are drawn about the point of intersection with their radii proportional to n and n′, the refractive indices before and after the surface, respectively. From the intersection of the ray with circle n at point A, a line is drawn parallel with the normal until it intersects circle n′ at point B. The refracted ray is then drawn through

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307

Example A—Raytrace Data R c  1/R t n

50.0 0.020 1.00

15.0 1.50

50.0 0.020 1.00

Paraxial Calculation given: u1  0.1 l1  200.0 y1  20.0 (by 10.1a) y by 10.1d 20.0 19.0 u by 10.1c 0.1 0.066667 0.29 l′ by 10.1f 65.517241 Meridional Calculation given: sin U1  0.1 L1  200.0 Q1  20.0 (by 10.2a) Q by 10.2g 20.0 19.589064 sin l by 10.2c 0.5 0.475278 sin I′ by 10.2d 0.333333 0.712918 sin U′ 0.1 0.083497 0.372744 cos U′ 0.9949874 0.996508 0.927934 Q′ by 10.2f 20.841522 17.008692 L′ by 10.2i H′ (s′l′) by 10.2j 45.631041 7.988131

Figure 10.3 Graphical raytrace.

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point B and the ray-surface intersection. (For reflection, n′  n, and a single circle is drawn. Point B is located at the intersection of the parallel and the index circle on the opposite side of the surface. If desired, the index circle construction can be carried out off to one side of the drawing (to avoid cluttering the diagram) and the angles transferred to the drawing. An alternative is to measure the angle of incidence and compute the angle of refraction using Snell’s law (n sin I  n′ sin I′). The accuracy of graphical raytracing is poor and the process is laborious. Thus, it is rarely used except for crude condensertype design. It is usually preferable to use a computer and draw the rays from the computed data, or, better yet, to have the computer draw the whole thing. 10.4 General, or Skew, Rays: Spherical Surfaces A skew ray is a perfectly general ray; however, the application of the term “skew” is usually restricted to rays which are not meridional rays. A skew ray must be defined in three coordinates x, y, and z, instead of just z and y as in the case of meridional rays. Until the advent of the electronic computer, skew rays were rarely traced because of the lengthy computation involved. Since a skew ray takes only a bit longer to trace on an electronic computer than a meridional ray, the reverse situation is now common, and meridional rays are usually traced as special cases of general rays. The general raytracing equations given below are slightly modified from those presented by D. Feder in the Journal of the Optical Society of America, vol. 41, 1951, pp. 630–636. The ray is defined by the coordinates x, y, and z of its intersection point with a surface, and by its direction cosines, X, Y, and Z. The origin of the coordinate system is at the vertex of each surface. Figure 10.4 shows the meanings of these terms. Note that if x and X are both zero, the ray is a meridional ray and direction cosine Y equals sin U. The direction cosines are the projections, on the coordinate axes, of a unit-length vector along the ray. The direction cosines may be visualized as the length, height, and width of a rectangular solid or box which has a diagonal equal to one (1.0). (Note that the optical direction cosine is simply the direction cosine as defined above, multiplied by the index of refraction.) The computation is opened by determining the values for x, y, z, X, Y, and Z with respect to an arbitrarily chosen reference surface, which may be plane (the usual choice) or spherical. Convenient choices for the location of the reference surface are at the object (which allows the easy use of a curved object surface, if appropriate), at the vertex of the

Optical Computation

309

Figure 10.4 Symbols used in skew raytracing Eqs. 10.4a through 10.4p. (a) The physical

meanings of the spatial coordinates (x, y, z) of the ray intersection with the surface and of the ray direction cosines, X, Y, and Z. (b) Illustrating the system of subscript notation.

first surface, or at the entrance pupil. Note that Eq. 10.3a is simply the equation of a sphere (and thus assures that the ray origin point lies in the reference surface), and that Eq. 10.3b assures that the square of the unit vector along the ray is equal to 1.0. Opening (at the reference surface): c (x 2  y 2  z 2) 2z  0 2

2

2

X  Y  Z  1.0

(10.3a) (10.3b)

Transfer to the first (or next) surface: e  tZ (xX  yY  zZ)

(10.3c)

M1z  z  eZ  t

(10.3d)

M12  x 2  y 2  z2  e2  t 2  2tz

(10.3e)

E1 

 2M苶 兹苶 Z  c苶 1(c1M 苶 1z) 2 1

2

(10.3f)

(c1M122M1z) L  e   Z  E1

(10.3g)

z1  z  LZ  t

(10.3h)

y1  y  LY

(10.3i)

x1  x  LX

(10.3j)

Refraction: E′ 

冢 莦 冣 莦 冪莦莦 n 1  n1

2

(1  E12)

(10.3k)

310

Chapter Ten

n g1  E′1   E1 n1

(10.3l)

n Z1   Z  g1c1z1  g1 n1

(10.3m)

n Y1   Y  g1c1y1 n1

(10.3n)

n X1   X  g1c1x1 n1

(10.3o)

Terms without subscript refer to the reference surface and the following space. Terms subscripted with 1 refer to the first surface and the following space. The symbols have the following meanings: x,y,z

The spatial coordinates of the ray intersection with the reference surface.

x1,y1,z1

The spatial coordinates of the ray intersection with surface #1.

M1

The distance (vector) from the vertex of surface #1 to the ray, perpendicular to the ray.

M1z

The z component of M1.

E1

The cosine of the angle of incidence at surface #1.

L

The distance along the ray from the reference surface (x, y, z) to surface #1 (x1, y1, z1). Lj is the distance from surface j to j1.

E′1

The cosine of the angle of refraction (I′) at surface #1.

X,Y,Z

The direction cosines of the ray in the space between the reference surface and surface #1 (before refraction).

X1,Y1,Z1

The direction cosines after refraction by surface #1.

c

The curvature (reciprocal radius  1/R) of the reference surface.

c1

The curvature of surface #1.

n

The index between the reference surface and surface #1.

n′

The index following surface #1.

t

The axial spacing between the reference surface and surface #1.

Notice that the choice of the positive value for the square root in Eq. 10.3f selects that intersection of the ray with the surface which is nearer the surface vertex. Also, if the argument under the radical in Eq. 10.3f is negative, it indicates that the ray misses (never intersects) the spherical surface. If the argument under the radical in Eq. 10.3k is negative, it indicates that the angle of incidence exceeds the critical

Optical Computation

311

angle; the ray is thus subject to total internal reflection (TIR) and cannot pass through the surface. The calculation is opened by inserting c, two of the coordinates (x, y, z), and two of the direction cosines (X, Y, Z) into Eqs. 10.3a and b and solving for the third coordinate and the third direction cosine. Then the intersection of the ray with the first surface (x1, y1, z1) is determined from Eqs. 10.3c through 10.3j. Next the ray direction cosines after refraction at surface #1 (X1, Y1, Z1) are found from Eqs. 10.3k through 10.3o. This completes the raytrace through the first surface; at this point Eqs. 10.3a and 10.3b (with unit subscripts) may be used to check the accuracy of the computation. To transfer to the second surface, the subscripts of Eqs. 10.3c through 10.3j are advanced by one, and x2, y2, and z2 are determined. Similarly, the direction cosines after refraction (X2, Y2, Z 2) at surface #2 are found by Eqs. 10.3k through 10.3o with the subscripts incremented. This process is repeated until the intersection of the ray with the final surface of the system, which is usually the image plane, has been determined. This completes the calculation. Note that any ray which intersects the axis is a meridional ray; thus it is only necessary to trace skew rays from off-axis object points. Further, there is no loss of generality in assuming that the object point lies in the yz plane of the coordinate system (because we assume a system with axial symmetry). Therefore, any skew ray can be started with x equal to zero. When this is done, it is apparent that the two halves of the optical system, in front of, and behind the y  z plane are mirror images of each other and that any ray Xk , Yk , Z k passing through xk, yk, zk has a mirror image (Xk), Yk, Zk passing through (xk), yk, zk in the other half of the system. For this reason, it is only necessary to trace skew rays through one-half of the system aperture; rays through the other half are represented by the same data with the signs of x and X reversed. Example B

Using the lens of Example A, we will trace a skew ray originating in the object plane (200 mm to the left of the lens) at a point 20 mm above the axis. Thus, the ray intersection coordinates in the reference plane (in this case, the object plane) are x  0, y  20, z  0. If we set Y  0.1 and X  0.1, the ray will intersect the first surface of the lens approximately in the xz plane, about 20 mm in front of the (optical) z axis. For the image surface we will use the paraxial focal plane as computed in Example A. The calculation is shown in the table on the next page.

312

Chapter Ten

Example B—Skew Trace through a Sphere First surface

Object plane R c t n Transfer: e by 10.3c Mz by 10.3d M2 by 10.3e E by 10.3f L by 10.3g z by 10.3h y by 10.3i x by 10.3j Refraction: E′ by 10.3k g by 10.3l Z by 10.3m Y by 10.3n X by 10.3o Check: zero by 10.3a 1.0 by 10.3b

0.0

Second surface

50 0.02 200. 1.0

Image plane

50 0.02 15. 1.50

0.0 65.517241 1.0

199.989899 2.0201011 404.040418 0.8588247 206.546141 4.470247 0.654614 20.654614

12.188013 1.590643 389.369720 0.8772472 6.327736 4.237125 1.046031 20.116291

(0.9899495) (0.1) (0.1)

0.9398771 0.3673272 0.9944527 0.0618575 0.0850734

0.6939135 0.6219573 0.9224280 0.0797745 0.3778396

(0.0) (1.0)

0.0000001 1.0000000

0.0000015 1.0000001

(0.0) (20.0) (0.0)

71.860665 3.468077 107.475746 0.9224280 75.620392 0.000000 7.078610 8.456088

10.5 General, or Skew, Rays: Aspheric Surfaces For raytracing purposes, an aspheric surface of rotation is conveniently represented by an equation of the form cs2 z  f(x, y)    A2s 2  A 4s 4  ...  A j s j s2] [1  兹苶 1  c 2苶

(10.4a)

where z is the longitudinal coordinate (abscissa) of a point on the surface which is a distance s from the z axis. Using the same coordinate system as Sec. 10.4, the radial distance s is related to coordinates y and x by s2  y2  x2

(10.4b)

As shown in Fig. 10.5, the first term of the right-hand side of Eq. 10.4a is the equation for a spherical surface of radius R  1/c. The subsequent terms represent deformations to the spherical surface, with A2, A4, etc., as the constants of the second, fourth, etc., power deformation terms. Since any number of deformation terms may be included, Eq. 10.4a is quite flexible and can represent some rather extreme aspher-

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313

Figure 10.5 Showing the signifi-

cance of Eq. 10.4a, which defines an aspheric surface by a deformation from a reference spherical surface. The z coordinate of a point on the surface is the sum of the z coordinate of the reference sphere and the sum of all the deformation terms.

ics. Note that Eq. 10.4a is redundant in that the second-order deformation term (A2s2) is not necessary to specify the surface, since it can be implicitly included in the curvature c. The importance of the inclusion of this term is that otherwise a large value of c (i.e., a short radius) could be required to describe the surface, and rays which would actually intersect the aspheric surface might not intersect the reference sphere. As can be seen from Example C, if necessary the reference sphere may be a plane. Aspheric surfaces which are conic sections (paraboloid, ellipsoid, hyperboloid) also can be represented by a power series; see Sec. 13.5 for further details. The difficulty in tracing a ray through an aspheric surface lies in determining the point of intersection of the ray with the aspheric, since this cannot be determined directly. In the method given here, this is accomplished by a series of approximations, which are continued until the error in the approximation is negligible. The first step is to compute x0, y0, and z0, the intersection coordinates of the ray with the spherical surface (of curvature c) which is usually a fair approximation to the aspheric surface. This is done with Eqs. 10.3c through 10.3j of the preceding section. Then the z coordinate of the aspheric (z苶0) corresponding to this distance from the axis is found by substituting s02  y02x02 into the equation for the aspheric (10.4a) z 0  f (y0, x 0) 苶

(10.4c)

314

Chapter Ten

Then compute 1  c 2苶 s 02 l0  兹苶

(10.4d)

m0  y0[c  l0(2A 2  4A 4s 0  ...  jA j s0 )] n0  x0[c  l0(2A2  4A 4 s02  ...  jA j s 0 (j2))] 2

l0 (z苶0  z0) G0   (Xl0  Ym0  Zn0)

(j2)

(10.4e) (10.4f) (10.4g)

where X, Y, and Z are the direction cosines of the incident ray. Now an improved approximation to the intersection coordinates is given by (10.4h) x1  G0 X  x0 y1  G0Y  y0

(10.4i)

z1  G0 Z  z0

(10.4j)

The process is sketched in Fig. 10.6. The approximation process is now repeated (from Eq. 10.4c to 10.4j) until the error is negligible, i.e., until (after k times through the process) (10.4k) zk  z苶k to within sufficient accuracy for the purposes of the computation.

Figure 10.6 Determination of the ray intersection with an aspheric

surface. The intersection is found by a convergent series of approximations. Shown here are the relationships involved in finding the first approximation after the intersection with the basic reference sphere has been determined.

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315

The refraction at the surface is carried through with the following equations: P 2  l k2  m k2  n k2

(10.4l)

F  Z l k  Ym k  Xn k

(10.4m)

F′ 

冣 冢 冪莦莦 莦莦 莦 n2 n2 P2 1 2  2 F 2 n1 n1

(10.4n)

1 n g  2 F′   F P n1

(10.4o)

n Z1   Z  gl k n1

(10.4p)

n Y1   Y  gm k n1

(10.4q)

n X1   X  gn k n1

(10.4r)

冢

冣

This completes the trace through the aspheric. The spatial intersection coordinates are xk, yk, and zk, and the new direction cosines are X1, Y1, and Z1. Example C

As a numerical example, let us trace the path of a ray through a paraboloidal mirror. The equation of a paraboloid with vertex at the origin is s2 z  4f and if we choose a concave mirror with a focal length of 5, the constants of Eq. 10.4a become c  0, A2  1/(4f)  0.05, and A4, A6, etc., equal zero. Thus z  0.05s2  0.05 (y2  x2) We will place the initial reference plane at the vertex of the parabola and the final reference (image) plane at the focal point. Thus t  0 and t1  f  5 (following our usual sign convention for distance after reflections). We will trace the ray striking the reference plane at z  0, y  0, x  1.0 at a direction of Y  0.1, X  0, and (by Eq. 10.3b)

316

Chapter Ten

Z  0.9949874. The index of refraction before reflection n equals 1.0 and the index after reflection n1 will then be 1.0, again following the convention of reversed signs after reflection. The computation is indicated in the following tabulation, where the applicable equation number is given in parentheses at each step. The steps indicated by (10.4d) through (10.4c) are repeated top to bottom until 苶zk  zk to (in this instance) seven places past the decimal. The fact that this example converged in only two cycles despite the fact that c  0 is a poor approximation to our paraboloid, is an indication of the rapidity of convergence of this technique. Reference surface: c0  0 t0  0.0

n0  1.0

Aspheric: z  0.05s2 c1  0 A2  0.05 (A4, etc.  0) t1  5.0

n1  1.0

Image surface: c2  0 Given: z  0, y  0, x  1.0 Z  0.9949874 Y  0.10 X  0.0 Since c  0 for the aspheric, it is obvious that z0  z  0, y0  y  0, and x0  x  1.0. Thus, z苶0  0.05(y2x2)  0.05 (by Eq. 10.4c) and 苶z0z0  0.05. (The same results can be obtained from Eqs. 10.3c through j) Intersection of Ray with Aspheric: (10.4d)

l0  1.0

l1  1.0

(10.4e)

m0  0.0

m1  0.0005025

(10.4f)

n0  0.1

n1  0.1

(10.4g)

G0  0.0502519

G1  0.0000013

(10.4h)

z1  0.050

z2  0.0500013

(10.4i)

y1  0.0050252

y2  0.0050253

(10.4j)

x1  1.0

x2  1.0

(10.4c)

z苶1  0.0500013 z苶1z1  0.0000013

z苶2  0.0500013 z苶2z2  0.0000000

Refraction: (10.4l)

P2  1.0100002

(10.4m)

F  0.9949372

(10.4n)

F′  0.9949372

(10.4o)

g  1.9701722

(10.4p)

Z1  0.09751848

(10.4q)

Y1  0.1009900

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(10.4r)

317

X1  0.1970172 X12Y12Z12  1.0000001

Intersection of Ray with Image Surface: (10.3c)

e1  5.0246880

(10.3d)

M2z  0.0499993

(10.3e)

M22  0.2550229

(10.3f)

E2  0.9751848

(10.3g)

L2  5.0759596

(10.3h)

z2  0

(10.3i)

y2  0.5075959

(10.3j)

x2  0.0000513

10.6 Coddington’s Equations The tangential and sagittal curvature of field can be determined by a process which is equivalent to tracing paraxial rays along a principal ray, instead of along the axis. In Chap. 3 it was pointed out that the slope of the ray intercept plot was equal to Zt, the tangential field curvature. This slope could be determined by tracing two closely spaced meridional rays and computing H′1H′2  H′ Zt     tan U′2tan U′1

tan U′ and a similar process using close sagittal (skew) rays would yield Zs, the sagittal field curvature.* Coddington’s equations are equivalent to tracing a pair of infinitely close rays, and the formulation has a marked similarity to the paraxial raytracing equations. However, object and image distances as well as surface-to-surface spacings are measured along the principal ray instead of along the axis, and the surface power is modified for the obliquity of the ray. Figure 10.7 shows a principal ray passing through a surface with sagittal and tangential ray fans originating at an object point and converging to their focii. The distance along the ray from the surface to the focus is symbolized by s and t for the object distance and by s′ and t′ for the image distance. The sign convention is as usual; if the focus or object point is to the left of the surface, the distance is negative; to the right, positive. In Fig. 10.7, s and t are negative, s′ and t′ are positive.

*Note that despite the currently almost universal use of z to represent the optical axis, it is still common usage to symbolize field curvature as xt and xs.

318

Chapter Ten

Figure 10.7

The computation is carried out by tracing the principal ray through the system using the meridional formulas of Sec. 10.3, determining the oblique power for each surface by   c (n′ cos I′  n cos I)

(10.5a)

and determining the distance (D) from surface to surface along the ray by Eq. 10.2m. The initial values of s and t are determined (Eq. 10.2m is often useful in this regard) and then the focal distances are determined by solving the following equations for s′ and t′. n′ n     s′ s

(sagittal)

n cos2 I n′ cos2 I′      t′ t

(tangential)

(10.5b) (10.5c)

The values of s and t for the next surface are given by s2  s′1  D

(10.5d)

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319

(10.5e)

t2  t′1  D

where D is the value given by Eq. 10.2m. The calculation is repeated for each surface of the system; the final values of s′ and t′ represent the distances along the ray from the last surface to the final foci. The final curvature of field (with respect to a reference plane an axial distance l′ from the last surface) can be found from zs  s′ cos U′  z  l′

(10.5f)

zt  t′ cos U′  z  l′

(10.5g)

where z is determined for the last surface by Eq. 10.2l. The preceding equations are ill-suited for use on an electronic computer, since s and t may be too large for the machine capacity, or too small (so that 1/s and 1/t become large). The following equations have been developed to avoid this difficulty. They make use of ys and yt, which are fictional ray heights from the principal ray (analogous to the paraxial ray heights used in Eqs. 10.1) and equally fictional ray slopeindex products Ps and Pt with respect to the principal ray. The calculation is again begun by tracing a principal ray. The opening equations are nys Ps   (10.5h) s nyt cos 2 I Pt   t

(10.5i)

where the data refer to the first surface of the system, and ys and yt are arbitrarily chosen. The ray slope-index product after refraction is determined from P ′s  Ps  ys

(10.5j)

P′t  Pt  yt

(10.5k)

where  is the oblique surface power given by Eq. 10.5a. The “ray height” at the next surface is given by (P ′s)1D ( ys) 2  ( ys) 1   n′1

冤

cos2 I ′1 (P ′t)1D (yt) 1   (yt) 2   cos 2 I 2 n′1 cos 2 I ′1

(10.5l)

冥

(10.5m)

At surface #2, the incident ray slope-index product is given by P2  P ′1.

320

Chapter Ten

This process is repeated for each surface of the system, and the final image distances at the last surface are found from: n′ys s′   P′s

(10.5n)

n′yt cos2 I ′ t′   P ′t

(10.5o)

The final curvature of field is found from Eqs. 10.5f and g. Example D

We will use the meridional ray traced in Example A as the principal ray and trace close sagittal and tangential rays about it, assuming that the object point is at the axial intercept of the ray, i.e., on the axis and 200 mm to the left of the first surface. (From a practical standpoint, this will be equivalent to determining the imagery of the lens when used with a small pinhole diaphragm located 20 mm (radially) away from the axis.) To find the initial values for s and t, we determine z at the first surface by Eq. 10.2l (using the raytrace data from Example A for the first surface). Then 200  4.415778 lz s  t      205.445587 cos U 0.994987 The oblique surface powers are determined from Eq. 10.5a as 1  0.02 (1.5  0.942809  1.0  0.866025)   0.0109638 2  0.02 (1.0  0.701248  1.5  0.879835)   0.0123701 Equation 10.2m gives the distance along the ray between surfaces as 15.0  4.415778  (4.177626) D    6.429045 0.996508 then for the first surface 1.5 1     0.0109638 s′ 205.445 s′   246.0488 1.5 (0.942809)2 0.750     0.0109638 t′ 205.445

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321

t′  182.3186 We transfer to surface #2 by Eqs. 10.5d and e to get s2  239.6198 t2  175.8896 Then using Eqs. 10.5b and c for the second surface 1 1.5     0.0123701 s′ 239.6198 s′2   53.6768 1.161164 0.491748     0.0123701 t′ 175.8896 t′2   25.9200 By setting l′ in Eqs. 10.5f and g equal to 45.6310 (the final intercept of the marginal ray traced in Example A), we find that, with respect to this point, zs  49.80864.177645.6310  0.00 zt  24.05214.177645.6310  25.7565 One may gain an understanding of this rather interesting result by sketching the path of a few rays in a system of the type we have raytraced, remembering that a simple biconvex lens is afflicted with a large undercorrected spherical aberration. Alternatively, a study of the ray intercept curve for undercorrected spherical (with coordinates rotated to account for the shift of the reference plane to the focus of the marginal ray) will indicate the meaning of the value of zt found above. 10.7

Aberration Determination

This section will briefly indicate the computational procedures involved in determining the numerical values of the various aberrations discussed in Chap. 3. Since this discussion will be somewhat condensed, the reader may wish to review Chap. 3 at this point. We will assume that the paraxial focal distance l′ (from the vertex of the last surface of the system to the paraxial image) has been determined. It is also useful to predetermine the size and location of the entrance pupil.

322

Chapter Ten

Spherical aberration

Trace a marginal meridional ray from the axial intercept of the object (through the edge of the entrance pupil of the system) and determine its final axial intercept L′ and/or its intersection height H′ in the paraxial focal plane. Then the longitudinal spherical aberration (LA′) is given by LA′  L′  l′

(10.6a)

and the transverse spherical aberration (TA′) is given by TA′  H′  (LA′) tan U′

(10.6b)

The spherical aberration is overcorrected if the sign of nLA′ is positive and undercorrected if the sign is negative. The zonal spherical aberration is determined by tracing a second ray through the 0.707 zone (i.e., a ray which strikes the entrance pupil at a distance from the axis equal to 0.707 times the distance for the marginal ray). The zonal aberration is found from Eqs. 10.6a and b. Rays may also be traced through other zones of the aperture if a more complete description of the axial correction of the system is required. The 0.5 zone for zonal rays derives from customary choice of the 0.707  兹苶 the fact that, for most systems, the longitudinal spherical can be approximated by LA′  aY 2  bY 4

(10.6c)

where Y is the ray height and a and b are constants. Thus, if the marginal spherical, at a ray height of Ym, is corrected to zero, the maximum longitudinal zonal aberration occurs at Y

冪莦

Ym2   0.707Ym 2

The maximum transverse spherical TA′ occurs at Y

兹苶 0.6Ym2苶  0.775Ym

Coma

Three meridional rays are traced from an off-axis object point: a principal ray through the center of the entrance pupil and upper and lower rim rays through the upper and lower edges of the pupil. The final intersection heights of these rays with the paraxial focal plane are determined. Then the tangential coma is given by

Optical Computation

(H′A  H′B) (tan U′A  tan U′p) Coma T  H′A  H′p   (tan U′B  tan U′A)

323

(10.6d)

For most lenses, where the ray slope U′ is a smooth uniform function of the ray position in the pupil, the following simplified equation is sufficiently accurate. This can be evaluated when examining a ray intercept plot by connecting the ends of the plot with a straight line and noting the distance from the height of the principal ray intersection to the line. H′A  H′B Coma T    H′p 2 where H′p is the intercept for the principal ray and H′A and H′B are the intercepts of the rim rays. Ordinarily, sagittal coma is very nearly equal to one-third of the tangential coma (especially near the axis). Sagittal coma can be determined by tracing a skew ray through the entrance pupil at y  0, x  the radius of the pupil. Then the displacement of the y intersection coordinate in the image plane from H′p gives the sagittal coma (note that in this instance the image plane should be the plane of intersection of the upper and lower rim rays, i.e., where H′A  H′B). The variation of coma with field angle (or image height) can be determined by repeating the process for another object height. The variation of coma with aperture is found by tracing zonal oblique rays. OSC

The offense against the (Abbe) sine condition (OSC) is an indication of the amount of coma present in regions near the optical axis. It is determined by tracing a paraxial and a marginal ray from the axial object point and substituting their data into (l′  l′p) sin U u′ OSC      1 (L′  l′p) u sin U′

(10.6e)

where u and u′ are the initial and final slopes of the paraxial ray, U and U′ are the initial and final slopes for the marginal ray, l′ and L′ are the final intercept lengths of the paraxial and marginal rays, and l′p is the final intercept of the principal ray (thus l′p is the distance from the last surface to the exit pupil). If the object is at inifinity, the initial y and Q are substituted for u and sin U in 10.6e. For regions near the axis Comas  H′ (OSC) Coma t  3H′ (OSC)

(10.6f)

324

Chapter Ten

Distortion

Distortion is found by tracing a meridional principal ray from an offaxis object point through the center of the entrance pupil and determining its intersection height H′p in the paraxial focal plane. A paraxial principal ray may be traced from the same object point to determine the paraxial image height h′, or the optical invariant I may be used as indicated in Chap. 2. Distortion  H′p  h′

(10.6g)

Distortion is frequently expressed as a percentage of the image height, thus: H′ph′ Percent distortion    100 h′

(10.6h)

The variation of distortion with image height or field angle is found by repeating the process for several object heights. Astigmatism and curvature of field

Trace a principal ray from an off-axis object point through the center of the entrance pupil. Then trace close sagittal and tangential rays by Coddington’s equations (Sec. 10.6) and determine the final z′s and z′t with respect to the paraxial image plane; z′s and z′t are then the sagittal and tangential curvature of field for this image point. Alternatively, a meridional ray from the object point passing through the system close to the principal ray can be traced. Then H′pH′ Z t   tan U′tan U′p

(10.6i)

will provide a close approximation to z′t, since Z′t approaches z′t, as the two rays approach each other. A similar procedure with a close skew ray will yield Z′s. Since the variation of field curvature with image height is usually of interest, z′s and z′t may be determined for additional object heights or field angles and plotted against obliquity. Note that it is common to refer to the field curvature (zs and zt) as xs and xt, in conformance with earlier usage when the optical axis was denoted as the x axis.

Optical Computation

325

Chromatic aberration—Axial (or longitudinal)

Paraxial longitudinal chromatic aberration is found by determining the paraxial image points for the longest and shortest wavelengths of light in the spectral bandpass of the system. This is done by determining l′ using the indices of refraction associated with one wavelength and then with the other. For visual systems, the long wavelength is usually taken as C-light (  0.6563 m hydrogen line) and the short wavelengths as F-light (  0.4861 m hydrogen line). The longitudinal chromatic aberration is then LchA′  l′F  l′C

(10.6j)

The transverse measure of axial chromatic can be found from TAch  LchA tan U′K or by calculating the height of the rays in the mid-wavelength focal surface and TAch  h′F  h′C The chromatic aberrations for other zones of the aperture are found by tracing meridional rays from the axial object point for each wavelength and substituting the final axial intercepts into Eq. 10.6j. The secondary spectrum is found by tracing axial rays in at least three wavelengths—long, middle, and short—and plotting their axial intercepts against wavelength. A numerical value for the secondary spectrum is strictly valid only when the long and short wavelength images are united at a common focus, so that l′F  l′C then SS′  l′d  l′F  l′d  l′C

(10.6k)

where the subscripts C, d, and F indicate long, middle, and short wavelengths. For visual work, C, F, and d represent the C and F lines of hydrogen and the helium d line at 0.5876 m. The spherochromatism (chromatic variation of spherical aberration) is found by determining the spherical aberration at various wavelengths. Thus, for visual work the spherochromatism would be the spherical in F light minus the spherical in C light.

326

Chapter Ten

Chromatic aberration—Lateral

Lateral chromatic aberration, or chromatic difference of magnification, is determined by tracing a principal ray from an off-axis object point through the center of the entrance pupil in both long and short wavelengths and finding the final intersection heights with the focal plane. Then TchA  H′F  H′C

(10.6l)

for visual work. Alternatively, the paraxial lateral color can be found by tracing paraxial “principal” rays in two colors and substituting h′F and h′C into Eq. 10.6l. The chromatic difference of magnification is given by CDM  TchA/h′ Lateral chromatic aberration should not be confused with the transverse expression for axial (longitudinal) chromatic aberration, which is given by TAch  H′F  H′C   (LchA) tan U′

(10.6m)

where the data are derived from rays traced from an object point on the optical axis. Optical path difference (wave-front aberration)

Recalling (from Chap. 1) that a wave front which forms a “perfect” image is spherical in shape and is centered about the image point, it is apparent that the aberration of an image formed by an optical system can be expressed in terms of the departure of the wave front from an ideal spherical wave front. The velocity of light in a medium of index n is given by c/n, where c is the speed of light in vacuum, and the time required for a point on a wave front to travel a distance D through the medium is nD/c. Thus, if a number of rays from an object point are traced through an optical system, and the distances along each ray from surface to surface are computed (by Eqs. 10.2m or 10.4g), including the distance from object point to the first surface, then the points for which nD/c, or nD, are equal, are points through which the wave front passes at the same instant. A smooth surface through these points is the locus of the wave front. Referring to Example D, the distance along the ray from the object point to the first surface was computed as 205.446 mm. The distance from surface 1 to surface 2 was D  6.429 mm, and the distance from surface 2 to the axial intercept of the ray was S′2  53.677.

Optical Computation

327

If we now multiply each distance by the index (1.0, 1.5, and 1.0, respectively) and sum the products, we find that the optical path is nD  268.766 The calculation can be repeated for a ray along the axis; the distances are 200 mm, 15 mm, and 45.631, and the optical path along the axis is nD  268.131 Since the axial path is shorter by some 0.635 mm, it is apparent that when the wave front reaches this point via the axis, it is still 0.635 mm from the point along the path described by the marginal ray. If we “back up” a bit (a fraction of a nanosecond) to the time when the wave front has just emerged from the lens and construct a reference sphere (or circle) about L′  45.631, it will be apparent that the departure of the wave front from the reference sphere is equal to the difference in the optical paths to the reference sphere. Thus the wave-front aberration or optical path difference (OPD) can be found by tracing rays from the object to the surface of a reference sphere centered on the image point and determining OPD  (nD)A  (nD)B

(10.6n)

Note that the choice of the reference image point location will have a great effect on the size of the OPD, since a shift of the reference point is equivalent to focusing (in the longitudinal direction) or to scanning the image plane for the point image (when shifting the reference point laterally). In the example cited, a reference sphere constructed about a point 55.57 mm from the last surface would represent a much better “fit” to the wave front, and the OPD about this point would represent (approximately) the minimum obtainable for the aperture represented by this ray. Although the example cited above showed an OPD of more than 1000 wavelengths of visible light, it should be noted that OPD is usually measured in wavelengths, or fractions thereof. For example, the Rayleigh criterion may be expressed as follows: An image will be “sensibly” perfect if there exists not more than one-quarter wavelength difference in optical path over the wave front with reference to a sphere centered at the selected image point. The numerical precision required to obtain significant results in an OPD calculation is higher than that required for ordinary raytracing. The OPD is customarily determined with respect to a spherical surface (centered about the reference point) with a radius equal to the distance from the exit pupil to the reference point.

328

Chapter Ten

10.8 Third-Order Aberrations: Surface Contributions* If an analytic expression is derived for the transverse aberration of a general ray with respect to a reference ray (i.e., the lateral separation of their intersections in a reference plane), the expression can be broken down into orders, or powers, of the ray parameters. The parameters usually chosen are: (1) the obliquity of the reference ray, and (2) the separation between the two rays at the pupil of the system; they correspond to: (1) image height, and (2) system aperture. The aberrations of the first order turn out to be those which can be eliminated by locating the reference point at the paraxial image. The firstorder aberrations are thus defects of focus or image size which vary linearly with aperture or obliquity, such as simple focusing or paraxial chromatic aberration (transverse axial color or lateral color). See. Sec. 3.2 and Eqs. 3.1 and 3.2. The third-order terms correspond to the primary aberrations. The term in y3 (where y is the semiaperture, or separation of the rays) has no h (image height) component and corresponds to spherical aberration. The term in y2h corresponds to coma. The term in yh2 represents the astigmatism and curvature of field, and the term in h3 is distortion. The portions of the total aberration represented by these terms are called the third-order aberrations. There will also be terms in y 5, y 4h, y 3h2, y 2h3, yh4, and h5 (which are called the fifth-order aberrations), as well as terms in seventh, ninth, and higher exponents. (Note that in European usage, third and fifth order are frequently referred to as primary and secondary aberration). The importance of these aberration contributions diminishes rapidly as the exponent increases, just as in the series expansion for the sine of an angle x3 x5 x7 sin x  x        ... 3! 5! 7! The analogy here is quite good, since for optical systems in which the sines of the angles involved can be satisfactorily represented by sin x  x, first-order (paraxial) optics, which are based on just this approximation, are entirely adequate to describe the imagery. For systems with larger angles, more terms of the expansion are necessary to adequately describe the imaging properties, and the third- (or higher-) order aberration contributions must be taken into account. *D. Feder, “Optical Calculations with Automatic Computing Machines,” J. Opt. Soc. Am., vol. 41, pp. 630–636 (1951).

Optical Computation

329

Thus a knowledge of just the paraxial and third-order characteristics frequently yields a fair approximation to the performance of a system which is modest in aperture and angular coverage. In systems where this approximation is poor, the third-order contributions are nonetheless of value. Even in systems where the fifth and higher orders are appreciable, the higher orders tend to change very slowly as the design parameters (radius, spacing, index) are varied, so that, although the first and third orders may be inadequate to fully describe the correction of the system, they are capable of indicating the changes which will be produced by moderate changes in the design parameters. For example, if a parameter change produced a change of x in a thirdorder aberration, one would expect that the change in the total aberration X (as determined by a trigonometric raytrace) would be very nearly equal to x, even though the third-order aberration x might be quite different than the trigonometric value X. Further, surfaces which make a large contribution to the third-order aberrations also tend to make a large contribution of the same sign to the higher-order aberrations, and a knowledge of the source of high-order residuals is frequently useful in eliminating them. The third-order aberration contributions* can be readily calculated from the data of two paraxial rays; an axial ray (from the axial intercept of the object through the rim of the entrance pupil) and a (paraxial) principal ray (from an off-axis object point through the center of the entrance pupil). These rays are traced by Eqs. 10.1a through 10.1g. In the following, the ray data of the axial ray will be symbolized by unsubscripted letters (y, u, i, etc.) and that of the paraxial principal ray by letters with subscript p (yp, up, ip, etc.). The optical invariant Inv is determined from the data of the two rays at the first surface, or any convenient surface. Inv  yp nu  ynu p  hn′k u′k

(10.7a)

The final image height (i.e., the intersection point of the paraxial “principal” ray in the image plane) is determined from the principal ray or by Inv h  (10.7b) n′k u′k where n′k and u′k are the index and slope (of the axial ray) after passing through the last surface of the system. *The fifth, seventh, etc., orders may also be computed from paraxial raytrace data. Buchdahl develops specific equations by which the higher-order contributions may be calculated. The equations for the fifth-order contributions are very complex and are usually calculated as part of a computer optical software package.

330

Chapter Ten

Then the following are evaluated for each surface of the system: i  cy  u

(10.7c)

ip  cyp  up

(10.7d)

n(n′  n) B   y(u′  i) 2n′Inv

(10.7e)

n(n′  n) Bp   yp (u′p  ip) 2n′Inv TSC  Bi2h

(10.7f) (10.7g)

CC  Bii ph

(10.7h)

2

TAC  Bi p h

(10.7i)

(n  n′) chInv TPC   2nn′

(10.7j)

DC  h [B p ii p  1 2(u′p2  up2) ]

(10.7k)

yi n TAchC   n   n′ n′k u′k n′

冣

(10.7l)

yip n TchC   n   n′ n′ku′k n′

冣

(10.7m)

冢

冢

As previously, primed symbols refer to quantities after refraction at a surface. Most of the symbols (y, n, u, c) are defined in Sec. 10.2, or immediately above. Those which have not been previously defined are: B and Bp

Intermediate steps in the calculation.

i

The paraxial angle of incidence.

n

The dispersion of the medium, equal to the difference between the index of refraction for the short wavelength and long wavelength. For visual work, n  nF  nC, or n  (n  1)/V.

Inv

The optical invariant

The third-order aberration contributions of the individual surfaces are given by Eqs. 10.7g through 10.7m, where TSC

is the transverse third-order spherical aberration contribution.

CC

is the sagittal third-order coma contribution.

3CC

is the tangential third-order coma contribution.

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331

TAC

is the transverse third-order astigmatism contribution.

TPC

is the transverse third-order Petzval contribution.

DC

is the third-order distortion.

TAchC

is the paraxial transverse axial chromatic aberration contribution.

TchC

is the paraxial lateral chromatic aberration contribution.

Note that TAchC and TchC are first-order aberrations; since they are customarily computed at the same time as the third-order aberrations, the equations are presented here. The longitudinal values of the contributions may be obtained by dividing the transverse values by u′k, the final slope of the axial ray, thus TSC SC   u′k TAC AC   u′k TPC PC   u′k

(10.7n)

TAchC LAchC   u′k The Seidel coefficients can be obtained by multiplying the transverse third-order contributions or sums by (2n′ku′k). Thus S1  TSC (2n′ku′k) S2  CC (2n′ku′k) S3  TAC (2n′ku′k) S4  TPC (2n′ku′k) S5  DC (2n′ku′k) The third-order aberrations at the final image are obtained by adding together the contributions of all the surfaces to get TSC, CC, TAC, etc. These contribution sums are as follows: TSC

is the third-order transverse spherical aberration.

SC

is the third-order longitudinal spherical aberration.

CC

is the third-order sagittal coma.

3CC

is the third-order tangential coma.

332

Chapter Ten

TAC

is the third-order transverse astigmatism.

AC

is the third-order longitudinal astigmatism.

TPC

is the third-order transverse Petzval sum.

PC

is the third-order longitudinal Petzval sum.

DC

is the third-order distortion.

TAchC

is the first-order transverse axial color.

LchC

is the first-order longitudinal axial color.

TchC is the first-order lateral color.

To the extent that the first- and third-order aberrations approximate the complete aberration expansions, the following relationships are valid: SC ≈ L′  l′

(spherical)

3CC ≈ 1 2 (H′A  H′B)  H′p

(tangential coma)

zs ≈  P C   AC

(sag. curvature of field, xs)

zt ≈  P C  3 AC

(tan. curvature of field, xt)

h2 !  2PC

(Petzval radius of curvature)

100DC  ≈ percentage distortion h LAchC ≈ l′F  l′C TchC ≈ h′F  h′C

(axial color) (lateral color)

Contributions from aspheric surfaces

For the purposes of computing the third-order contributions, we can assume that the aspheric surface is represented by a power series in s2 z  1 2Ce s2  (1 8Ce3  K) s4  ...

(10.7o)

in which the terms in s6 and higher may be neglected. For aspheric surfaces given in the form of Eq. 10.4a, the equivalent curvature Ce and equivalent fourth-order deformation constant K may be determined from C e  c  2A 2

(10.7p)

A2 K  A 4   (4A 22  6cA 2  3c2) 4

(10.7q)

Optical Computation

333

where c, A2, and A4, are the curvature and second- and fourth-order deformation terms, respectively, of Eq. 10.4a. Note that if A2 is zero, Ce  c and K  A4; see Sec. 13.5 for conics, where A4  "/8R 3. The aspheric surface contributions are determined by first computing the contributions for the equivalent spherical surface Ce using Eqs. 10.7g through m. Then the contributions due to the equivalent fourth-order deformation constant K are computed by the following equations and added to those of the equivalent spherical surface to obtain the total third-order aberration contribution of the aspheric surface. 4K (n′  n) W   Inv TSC a  Wy 4h

(10.7r) (10.7s)

CCa  Wy3yp h

(10.7t)

TACa  Wy2yp2h

(10.7u)

TPCa  0

(10.7v)

DCa  Wyyp3h

(10.7w)

TAchCa  0

(10.7x)

TchCa  0

(10.7y)

It is worth noting that if the aspheric surface is located at the aperture stop (or at a pupil), then yp  0, and the only third-order aberration that is affected by the aspheric term is spherical aberration. The Schmidt camera makes use of this by placing its aspheric corrector plate at the stop so that only the spherical aberration of the spherical mirror is affected by the plate. Conversely, if an aspheric is expected to affect coma, astigmatism, or distortion, it must be located a significant distance from the stop. Example E

We shall determine the third-order surface contributions of the simple biconvex lens of Example A. We have already traced an axial paraxial ray in this example; we shall add a paraxial principal ray from an object point 20 mm below the axis and assume that the entrance pupil is at the first surface. Thus the starting data for this ray will be yp  0 and up  0.1. We shall also assume that the lens is of crown glass with a V-value of 62.5 (and therefore n  0.008).

334

c t n y u i

Chapter Ten

0.02 1.0 by 10.1d by 10.1c by 10.7c

0.02

15.0 1.5

1.0

20.0 0.1

19.0 0.066667

0.5

0.29 0.446667

yp up ip

by 10.1d by 10.1c by 10.7d

0

B Bp TSC SC CC TAC AC TPC PC DC TAchC LchC TchC

by 10.7a Inv2.0 by 10.7b h′ 6.896552 by 10.7e 0.722222 by 10.7f 0.0 by 10.7g 1.245211 by 10.7n 4.294 by 10.7h 0.249042 by 10.7i 0.049808 by 10.7n 0.1717 by 10.7j 0.045977 by 10.7n 0.1585 by 10.7k 0.019157 by 10.7l 0.183908 by 10.7n 0.6342 by 10.7m 0.036782

by 10.1f l′65.517241

1.0

0.1

0.066667 0.1

0.09 0.046667

2.624375 0.025625 3.610979 12.452 0.377266 0.039416 0.1359 0.045977 0.1585 0.008922 0.234115 0.8073 0.024460

by 10.1g h′6.896552

TSC  4.856190 SC16.745 CC  0.128224 TAC  0.089224 AC  0.3077 TPC  0.091954 PC  0.3171 DC  0.010235 TAchC0.418023 LchC  1.4415 TchC  0.012322

Example F

To illustrate the use of the aspheric third-order contribution formulas, we shall demonstrate that the third-order spherical of a paraboloidal mirror is equal to zero for an infinitely distant object. The equation for a paraboloid is simply z  s2/4f, and in terms of Eq. 10.4a, c  0, A2  1 (4f ) and the higher-order constants (A4, A6, etc.) are all zero. Thus, by Eqs. 10.7p, q, and r, we find that 1 Ce   2f 1 K  3 64f 1 8K W    8f 3Inv Inv remembering that for a mirror in air n  1.0 and n′  1.0. Then Eq. 10.7s gives the contribution of the equivalent deformation constant as

Optical Computation

335

y4h    TSCa 8f 3Inv For an infinite object distance, the axial ray has a slope u  0; Eq. 10.1c gives us (using Ce)u′  y/f and Eq. 10.7c yields i  y/2f. Substituting these values into Eq. 10.7e, we get (1.0) (1.0  1.0) y y B   y    2 (1.0) Inv f 2f

冢

冣

y2   2fInv Now Eq. 10.7g gives the spherical aberration contribution of the equivalent sphere as y2 TSC   2fInv

h 冢 2f 冣 y

2

y4h   8 f 3Inv The contribution of the paraboloid mirror is given by the sum of TSC and TSCa; since they are equal in magnitude and opposite in sign, the sum is zero. Note that the demonstration did not specify that the paraboloid was concave (the more usual case); a convex paraboloid is equally free of spherical when used in this manner. And although we assumed the reflector to be in air for convenience, had we carried the indices n′  n through the calculation, the result would have been the same. 10.9 Third-Order Aberrations: Thin Lenses; Stop Shift Equations When the elements of an optical system are relatively thin, it is frequently convenient to assume that their thickness is zero. As we have previously noted, this assumption results in simplified approximate expressions for element focal lengths, which are nonetheless quite useful for rough preliminary calculations. This approximation can be applied to third-order aberration calculations; the results form a very useful tool for preliminary analytical optical system design. The following equations may be derived by application of the equations of the preceding section to a lens element of zero thickness.

336

Chapter Ten

The thin-lens third-order aberrations are found by tracing an axial and a principal ray through the system of thin lenses, in the manner outlined in Chap. 2. The equations used are u′  u  y

(10.8a)

y2  y1  du′1

(10.8b)

where u and u′ are the ray slopes before and after refraction by the element,  is the element power (reciprocal focal length), y is the height at which the ray strikes the element, and d is the spacing between adjacent elements. From Chap. 2 we also recall that the power of a thin element is given by   1/f  (n  1) (c1  c2)

(10.8c)

 (n  1) c where c  c1c2 and c1 and c2 are the curvatures (reciprocal radii) of the first and second surfaces of the element. After tracing the axial and “principal” rays through the system, the following are computed for each element

冢

u′ u v   or v′   y y

冣

yp Q  y

(10.8d) (10.8e)

where u and y are taken from the data of the axial ray and yp is from the principal ray data. Then the aberration contributions may be determined from the stop shift equations: TSC*  TSC CC*  CC  Q TSC

(10.8f) (10.8g)

TAC*  TAC  2Q CC  Q 2 TSC

(10.8h)

TPC*  TPC

(10.8i)

DC*  DC  Q(TPC  3TAC)  3Q 2CC  Q 3TSC TAchC*  TAchC TchC*  TchC  Q TAchC

(10.8j) (10.8k) (10.8l)

Optical Computation

337

The starred terms are the contributions from an element which is not at the stop—that is, one for which yp ≠ 0. The unstarred terms are the contributions from the element when it is in contact with the stop (and yp  0) and are given by the following equations: y4 TSC   (G1 c 3  G2 c 2c1  G3 c 2v  G4cc12  G5 cc1 v  G6 cv2) u′k y4   (G1 c3  G2 c2c2  G3 c2v′  G4cc22  G5cc2v′  G6cv′2) u′k

(10.8m)

CC  hy2(0.25G5 cc1  G7 cv  G8 c2)  hy2 (0.25G5 cc 2  G7cv′  G8 c 2)

(10.8n)

h2u′k TAC   2

(10.8o)

h2u′k TAC TPC     2n n

(10.8p)

DC  0

(10.8q)

y 2 TAchC   Vu′k

(10.8r)

TchC  0

(10.8s) 2

y P TSchC   Vu′k

(10.8t)

The symbols in the preceding have the following meanings: u′k

is the final slope of the axial ray (at the image).

h

is the image height (the intersection of the “principal” ray with the image plane).

V

is the Abbe V-number of the lens material, equal to (nd  1)/(nF  nC).

P

is the partial dispersion of the lens material, equal to (nd  nC)/(nF  nC).

G1

through G8 are functions of the lens material index, listed below.

TSC, CC, TAC, DC, TPC, TAchC, and TchC have the same meanings as in Sec. 10.8. TSchC is the transverse secondary spectrum contribution, equal to (l′d  l′C)(u′k). The transverse aberrations may be converted to longitudinal measure by dividing by (u′k) per Eq. 10.7n, as follows:

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Chapter Ten

TSC SC   u′k TAC AC   u′k TPC PC   u′k TAchC LchC   u′k TSchC SchC   u′k The relations between the thin-lens contributions and the various measures of the aberrations are the same as indicated in Sec. 10.8. n2 (n  1) G1   2

2 (n  1) (n  1) G5   n

(2n  1) (n  1) G2   2

(3n  2) (n  1) G6   2n

(3n  1) (n  1) G3   2

(2n  1) (n  1) G7   2n

(n  2) (n  1) G4   2n

n (n  1) G8   2

(10.8u)

The contributions, TSC*, CC*, etc., are determined for each element in the system. The individual contributions are then added to get TSC*, CC*, etc., and, to the extent that (1) the thin-lens fiction is valid, and (2) the third-order aberrations represent the total aberration of the system, SC ≈ L′  l′ CC* ≈ coma S PC*  AC* ≈ x s PC*  3 AC* ≈ x t

≈ 1 3coma T (sagittal field curvature) (tangential field curvature)

1   !  Petzval radius  n

Optical Computation

339

100 DC*  ≈ percentage distortion h LchC  l′F  l′C TchC*  hF  hC SchC  l′d  l′C The thin-lens third-order aberration expressions (which are frequently called G-sums) can be used with the specific data of an optical system to determine the (approximate) aberration values. Another usage is in design work where the curvatures and/or spacings and powers of the elements are to be determined in such a way that the aberration values are equal to some desired set of values, as will be evident in Chap. 12. For aspheric surfaced lenses, the contributions from the asphericity are calculated (by Eqs. 10.7r through 10.7y) and added to the contributions calculated for spherical surfaced lenses. Equations 10.8f to 10.8l are called stop shift equations. They may also be applied to the surface contributions (from Eqs. 10.7) to determine the third-order aberrations for a new, or changed, stop position by setting ( y*p  yp) Q   y where y*p is the ray height of the “new” principal ray (i.e., after the stop is shifted) and yp and y are as indicated in Sec. 10.8. Note that Q is an invariant; thus the values for y*p , yp , and y may be taken at any convenient surface. When the equations are used this way the unstarred terms (SC, CC, etc.) refer to the aberrations with the stop in the original position, while the starred terms (SC*, CC*, etc.) refer to the aberrations with the stop in the new position. Another consequence of the invariant nature of this definition of Q is the fact that the stop shift may be applied to either the individual surface contributions or to the contribution sums of the entire system or any portion thereof. The implications of the stop shift equations (Eqs. 10.8f through l) are worthy of note. If all the third-order aberrations are corrected for a given stop position, then moving the stop will not change them. Similarly, if there is no spherical, the coma is not affected by a stop shift. This is the case with the paraboloid mirror which, because it has no spherical aberration, has the same amount of coma regardless of where the stop is placed. But because it has coma, the astigmatism is a function of the stop position.

340

Chapter Ten

Example G

We will repeat Example E, assuming that the lens is thin. Since c1  0.02 and c2  0.02, the power of the thin lens is   (1.51)  (0.020.02)  0.02. For the axial ray u  0.1 and y  20; Eq. 10.8a gives u′  0.3, and, since there is only one element in the “system,” u′  u′k  0.3. The final image distance is 20/(0.3)  66.6 mm and the image height corresponding to an object height of 20 mm can be determined by h′  hu/u′  6.66 mm, or by tracing a paraxial principal ray. Applying Eqs. 10.8u, we find the G-functions corresponding to n  1.5 to be G5  1.666… G1  0.5625 G2  1.0

G6  1.08333…

G3  1.375

G7  0.666…

G4  0.5833…

G8  0.375

Thus we have the data (tabulated below for convenience) necessary to determine the “stop in contact” aberrations. y  20

y2  400

u′k  0.3

u′k2  0.09

c  0.04

c2  16  104

c1  0.02

c12  4  104

v  0.005

v 2  25  106

h  6.66…

h2  44.44…

y 4  160,000  16  104 c 3  64  106

V  62.5   0.02 We will use the first surface versions of Eqs. 10.8m and n; the second surface versions (data in c2 and v′) are primarily for use in analytical work with cemented doublets where it is desirable to express the aberration of the doublet as a function of the curvature of the cemented surface. 16  104 TSC   [0.5625  64  1061.0  16  104  0.02 0.3 1.375  16  104 ( 0.005)  0.5833  0.04  4  104  1.666  0.04  0.02 ( 0.005)  1.0833  0.04  25  106]

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TSC  5.333  105 [36  106  32  106  11  106  9.33  106  6.66  106  1.0833  106]  5.333  105 [10.0833  106]  5.3777… CC  6.666  400 [0.25  1.666  0.04  0.02  0.666  0.04 (0.005)  0.375  16  104]  2.666  103 [3.33  104  1.333  104  6  104]  2.666  103 [1.333  104]   0.3555… 44.44  0.02  (0.3) TAC   2  0.1333… 44.44  0.02  (0.3) TPC   2  1.5  0.0888… DC  0.0 400  0.02 TAchC   62.5  (0.3)  0.42666… TchC  0.0 The above are the third-order aberrations of our thin lens with the stop (pupil) at the lens; these results may be compared with Example E (where the stop was at the first surface). However, let us assume that the stop is 50 mm to the left of the lens. With the object height of 20 mm as before, this gives up  20/150  0.13333 and yp  20200(0.1333)  6.666. Thus, Eq. 10.8e gives Q  0.333 and we can determine the aberrations of the lens under these conditions from Eqs. 10.8f through l. TSC*  5.3777… CC*  0.3555  0.333 (5.3777)  1.4370

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Chapter Ten

TAC*  0.1333  2 (0.333)(0.3555)  (5.3777) (0.333)(0.333)  0.4938 TPC*  0.0888 DC*  0  (0.333) (0.0888  0.4)  3 (0.333)(0.333)(0.3555)  (0.333)(0.333)(0.333) (5.3777)  0.1629629  0.1185185  0.1991767  0.2436 TAchC*  0.42666… TchC*  0  0.333 (0.42666)  0.1422

Example H

As a final example for this chapter, we present a raytrace analysis of an air-spaced photographic triplet lens. The constructional data shown in Fig. 10.8 are taken from K. Pestrecov’s U.S. Patent No. 2,453,260 (1948). Although the data are for a focal length of 100, this lens is designed for use as an 8- or 16-mm movie camera objective of short focal length (i.e., f  1326 mm). The analysis is begun by determining the size and position of the entrance pupil. The patent gives a speed of f/2.7; thus the pupil diameter is 37 units, and, if we assume the stop to be at R4, the apparent position of the pupil is 25 units to the right of R1. For an object at infinity, the paraxial rays necessary for the third-order aberration calculation

Figure 10.8 Section drawing and constructional data for a triplet photographic objective

(f/2.7, focal length 100) from U.S. Patent No. 2,453,260 (1948-Pestrecov).

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343

are represented by u  0, y  18.5, up  0.25, and yp  6.3. The results are efl  100.0 bfl  79.34 TSC  0.422

CC  0.0017

DC  0.057

TAC  0.070

TAchC  0.059

TPC  0.272

TchC  0.021

Next, meridional rays are traced for the axial bundle (U  0) in C, D, and F light. For the marginal ray Q1  18.5 and for the zonal ray Q1  13.1. The results are plotted in Fig. 10.9; plot A shows transverse measure and plot F longitudinal measure. Principal rays are traced at several obliquities through the center of the pupil (so that Q/sin U  lpr  25.0) and Coddington’s equations

Figure 10.9 Aberration plots of f/2.7 triplet (see Fig. 10.8 for construc-

tional data). Plots (a), (b), (c), (d) are meridional ray intercept curves with H (in the paraxial focal plane) as ordinates and tan U′6 as abscissa. The dashed portions indicate rays cut off by vignetting. Plot (e) is one-half of a sagittal (skew) fan, with x as ordinate. Plot (f) shows the longitudinal spherical aberration (abscissa) as a function of the entering ray height. Plot (g) shows sagittal and tangential field curvature (abscissa) as a function of the final image height.

344

Chapter Ten

are applied to determine the field curvature, which is shown in plot G of Fig. 10.9. To compute the data for the ray intercept curves, a fan of meridional rays was traced at each obliquity. The starting data were chosen so that one ray (principal) passed through the center of the pupil and pairs of rays passed through the rims (Y  ±18.5), the 75 percent zones (Y  ±13.875) and the 50 percent zones (Y  ±9.25). For example, the starting values for Q for the bundle at 14.5° (sin U1  0.25) were 6.25 for the principal ray and 11.662548 and 24.162548 for the rays through the pupil rim. (These three rays are shown as dashed lines in Fig. 10.8). The seven final values of H′ (in the paraxial focal plane 79.3357 to the right of R6) are plotted against tan U′6. Note also that the slope of the plot through the point representing the principal ray is equal to Z T (Z T  dH′/d tan U′  Xt). A sketch of the system with the rays drawn in (as in Fig. 10.8) will indicate which rays do not get through the lens; in Fig. 10.9, we indicate this by dashing the vignetted portion of the ray intercept curve. We assumed a clear aperture of 37 at R1 and 32 at R6. A sagittal fan of three rays was traced with pupil intersections z  0, y  0, and x  18.5, 13.875, and 9.25. The final values of x in the image plane are plotted in Fig. 10.9e against the final ray direction cosine Z. The slope of this curve through the point (0, 0) can be obtained from z s  dx/d tan Uz  x s. A very minimal raytrace analysis might consist of the following: 1. Paraxial trace and third-order aberrations. 2. Marginal and zonal axial rays in three colors. 3. Coddington’s trace at full field and 0.7 field. 4. Tangential fan of five rays (including the principal ray used in 3) at full and 0.7 field, at least one fan in three colors. From this, one cannot only obtain the aberration plots of Fig. 10.9, but a number of other relationships such as: Variation of:

Spherical with obliquity Coma with obliquity Coma with aperture Distortion with obliquity Lateral color with obliquity

The completeness with which one must analyze a system varies greatly. Systems of large aperture or field angle will require a more complete analysis. Systems of small aperture and field may not even

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345

require a “zonal” analysis. If one is familiar with the general type of system under analysis, frequently the third-order aberrations plus a few carefully selected rays will yield an adequate picture of the system performance. Of course, a modern computer program delivers a complete analysis so easily that trying to minimize the amount of raytracing is not a very profitable way to spend one’s time. Bibliography Note: Titles preceded by an asterisk are out of print. Buchdahl, H., Optical Aberration Coefficients, Oxford, 1954. *Conrady, A., Applied Optics and Optical Design, Oxford, 1929. (This and vol. 2 also were published by Dover, New York.) Herzberger, M., Modern Geometrical Optics, New York, Interscience, 1958. Kingslake, R., Optical System Design, San Diego, Academic, 1983. Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (ed.), The Infrared Handbook, Washington, Office of Naval Research, 1985. *Welford, W., Aberrations of the Symmetrical Optical System, New York, Academic, 1974. Exercises Numerical exercises in optical computation tend to be excessively laborious, and when mistakes are made, the result is more often discouragement than enlightenment. Therefore, we suggest that the reader desirous of only a moderate amount of adventure scale the dimensional data of the numerical examples contained in this chapter by a convenient factor, say 0.5 or 2, and repeat the computations independently. For those who wish a bit more exercise, the following problems are based on the data of Example H and Fig. 10.8. The index of refraction data are as follows: nD

nF  nC

nC

nF

1.617 1.649

0.01123 0.01920

1.61370 1.64355

1.62493 1.66275

1 Determine the third-order aberrations. The initial ray data and answers are given in the second paragraph of Example H.

346

Chapter Ten

2 Trace principal rays in D, C, and F light with starting data Q  6.25, sin U  0.25. ANSWER:

H′D  25.8793, H′C  25.8720, H′F  25.8966

3 Trace close sagittal and tangential rays from an infinitely distant object by Coddington’s equations, using the D light principal ray of Exercise 2. ANSWER:

Zs(  Xs)  0.9528; Zt (  Xt)  0.4521

4 Trace a sagittal skew ray at obliquity sin U  0.25 (direction cosine Y  0.25) through the rim of the 37-diameter entrance pupil located 25 to the right of R1. ANSWER: Z  0.94805 Y  0.25941 X  0.18416 z  0 y  25.8657 x  0.0757

5 Sketch the appearance of the ray intercept curves of Fig. 10.9 (A, B, C, D, and E) in a plane 78.94 from R6 (i.e., 0.4 inside the paraxial focus). Note that this does not require additional raytracing.

Chapter

11 Image Evaluation

11.1

Introduction

In the preceding chapter we discussed the means by which ray paths are traced through an optical system and how the numerical values of the image aberrations may be determined. In this chapter, we will consider the interpretation of the results of such optical computations. The basic question to which we address ourselves is: “What effect does a given amount of aberration have on the performance of the optical system?” We have seen that raytracing yields an incomplete picture of the image-forming characteristics of a system, since the image formed by a “perfect” lens or mirror is not the geometric point that raytracing might lead us to expect, but a finite-sized diffraction pattern—the Airy disk and the surrounding rings. For small departures from perfection (i.e., aberrations which cause a deformation of the wave front amounting to less than one or two wavelengths) it is thus appropriate to consider the manner in which an aberration affects the distribution of energy in the diffraction pattern. For larger amounts of aberration, however, the illumination distribution as described by raytracing can yield a quite adequate representation of the performance of the system. Thus, it is convenient to divide our considerations into (1) the effects of small amounts of aberration, which we treat in terms of the wave nature of light, and (2) the effects of large amounts of aberration, which may be treated geometrically.

347

348

Chapter Eleven

11.2

Optical Path Difference: Focus Shift

We will begin our discussion of small amounts of aberration by determining the optical path difference (OPD) or wave-front deformation introduced by a longitudinal shift of the reference point. Figure 11.1 shows a spherical wave front (solid line) emerging from the pupil of a “perfect” optical system with a focus at point F. We wish to determine the OPD with respect to a reference point at R, which is some arbitrary distance  from F. If we construct a reference sphere (dashed), centered on R, which coincides with the wave front at the axis, then the OPD for a given zone (of radius Y) is the distance* from the reference sphere to the wave front measured along the radius of the reference sphere, as indicated in Fig. 11.1. From the figure we can see that, for modest amounts of OPD, the path difference is equal to the radius of the reference sphere (l  ) minus the radius of the wave front (l) all less  cos U. OPD   (l     cos Ul) n   (1cos U) To an approximation sufficient for our purposes, we can make the substitution cos U ≈ 1  1 2 sin2 U and the optical path difference resulting from a shift of the reference point by an amount  is given by OPD  1 2 n sin2 U

(11.1)

A longitudinal shift of the reference point is equivalent to defocusing the system; by use of Rayleigh’s quarter-wave criterion we can establish a rough allowance for the tolerable depth of focus. Setting the OPD equal to a quarter wavelength of light and solving for the permissible focus shift, Depth of focus   ±   2 (f/#)2 2n sin2 Um

(11.2a)

where is the wavelength of light, n is the index of the final medium, and Um is the final slope of the marginal ray through the system. Note that Um is used because the maximum amount of OPD occurs at the edge of the wave front. We can convert this to transverse measure by

*Times the index n of the final medium, if the final medium is not air.

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349

The optical path difference (OPD) introduced by a small longitudinal displacement () of the reference point is equal to the index (n) times [the radius of the reference sphere (l  ) minus the radius of the wave front (l) minus  cos U].

Figure 11.1

multiplying by the ray slope; using sin Um as a close enough approximation for the slope, we get Transverse /4 defocus, 0.5 0.5 H′      (f/#) NA n sin Um

(11.2b)

where NA  n sin Um and (f/#)  f-number. 11.3 Optical Path Difference: Spherical Aberration We begin by determining the OPD with respect to a reference sphere centered at the paraxial focus. In Fig. 11.2, the deformed wave front is shown as a solid line and the ray (normal to the wave front) from zone Y intersects the axis at point M. The reference sphere, centered at P, is shown dashed, and the OPD is, as before, the radial distance between the two surfaces times the index. Since the wave front is shown lagging behind the reference sphere, the sign of the OPD is shown negative, to be consistent. The ray is normal to the wave front and the radius is normal to the reference sphere; thus the angle  between the surface normals is also the angle between the surfaces, and, as indicated in the lower sketch, the change in OPD corresponding to a small change in height dY is given by the relation (dOPD)    n dY

350

Chapter Eleven

The OPD (with reference to the paraxial focal point) produced by spherical aberration. The small diagram indicates the relationship   (1/n) dOPD/dy. In the upper sketch, it is apparent that   LA sin U/l.

Figure 11.2

But the angular aberration  is also related to the spherical aberration by (LA) Y (LA) sin U      l l2 Combining and solving for dOPD we get Y n (LA) dY dOPD   l2 Now the longitudinal spherical aberration is a function of Y and can be represented by the series LA  aY 2  bY 4  cY 6  . . .

(11.3)

Making this substitution and integrating OPD  

冕

nY (aY 2  bY 4  cY 6  . . .) dY  l2

Y

0

n   2 l

冢

cY 8 aY 4 bY 6       ... 4 6 8

冣冨

Y 0

Image Evaluation

nY 2   2l2

冢

351

aY 2 cY 6 bY 4       ... 2 3 4

冣

cY 6 aY 2 bY 4  1 2 n sin2 U       . . . 2 3 4

冢

冣

(11.4)

Now Eq. 11.4 is the OPD with respect to the paraxial focus of the system. It is reasonable to expect that a more desirable reference point than the paraxial focus exists. Thus, by combining Eqs. 11.1 and 11.4, we get aY 2 bY 4 cY 6 1 2    OPD  2 n sin U     ... (11.5) 2 3 4

冤 冢

冣冥

which is the OPD with respect to an axial point a distance  from the paraxial focus. Third-order spherical aberration. In many optical systems, the spherical

aberration is almost entirely third-order; this is true for almost all systems composed of simple positive elements, and very nearly true for many other systems. Under such circumstances, Eq. 11.3 reduces to. LA  aY 2

(11.6)

OPD  1 2 n sin2 U [1 2 aY 2]

(11.7)

and Eq. 11.5 reduces to

Now at the edge of the aperture Y  Ym and LA  LAm; substituting these values into Eq. 11.6, we find that (for third-order spherical) LAm a  Ym2 and that 1 Y 1 OPD   n sin2 U   LAm  2 2 Ym

冤

冢 冣冥 2

(11.8)

To determine the value of  which will result in the smallest amount of OPD, we can try several values of  in Eq. 11.8 and plot the OPD for each as a function of Y. This has been done for shifts of   0, 1 2LAm, and LAm; the results are plotted in Fig. 11.3. It is apparent that the smallest departure from the spherical reference surface occurs when the OPD is zero at the margin. The corresponding shift of the reference point is LAm/2. Therefore, from the standpoint of wave-front aberration, the best focus is midway between the marginal and paraxial focal points.

352

Chapter Eleven

The OPD of a system with third-order spherical aberration, plotted as a function of Y for three positions of the reference point.

Figure 11.3

If we now substitute   LAm/2 into Eq. 11.8, we find (by differentiating with respect to Y and setting the result equal to zero) that the 苶  0.707 Ym and is given by maximum OPD occurs at Y  Ym 兹0.5 LA m OPD   n sin2 Um 16 This is one-quarter of the OPD at the paraxial focus. Applying Rayleigh’s criterion by setting the OPD equal to onequarter wavelength, we find the amount of marginal spherical aberration corresponding to this OPD is 4  16 (f/#)2 LAm   n sin2 Um

(11.9a)

Again, making an approximate conversion to transverse aberration by multiplying by sin Um, we get 4 4 TA m      8 (f/#) NA n sin Um

(11.9b)

Fifth-order spherical aberration. When the spherical aberration consists

of third and fifth order (and this includes the vast majority of all optical systems), we can write. LA  aY 2  bY 4 Substituting LA  LAm at Y  Ym and LA  LA z at Y  0.707 Ym, we find that the constants a and b are related to the marginal and zonal spherical by the following expressions:

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353

LA m  aYm2  bYm4 aYm2 bYm4 LA z     2 4 4LA zLA m a   Ym2 2LA m4LA z b   Ym4 The OPD is represented by truncating Eq. 11.5 1 aY 2 bY 4 OPD   n sin2 U     2 2 3

冢

冣

and the graph of OPD versus Y is a curve of the type shown in the upper plot of Fig. 11.4. The exact shape of the curve is, of course, dependent on the values of a, b, and . The best focus occurs when 3 (4LA zLA m)2 3a2 3        LA max 16b 32 (LA m2LA z) 4

OPD vs. Y in the presence of third- and fifth-order aberration. Upper: OPD is a sixth-order function of Y, its shape depending on the aberration coefficients, a and b, and the position of the reference point (). Middle: OPD vs. Y when   (3 4)LAmax Lower: OPD is minimized when LAm  0 and   (3 4)LAz.

Figure 11.4

(11.10)

354

Chapter Eleven

since at this point the OPD is zero for three values of Y as shown in the middle plot of Fig. 11.4. At this focus, the OPD at the margin is 3a2 aYm2 bYm4 1 OPDm   n sin2 Um      16b 2 2 3

冢

冣

(11.11)

and at the maximum (point x), which occurs at Y  Ym

 4b 冪莦莦 a

the OPD is given by na3 sin2 Um OPDx   96b2 Ym2

(11.12)

If the marginal spherical aberration of the system is corrected (so that LAm  0) then the values of OPD at the margin and at point X are equal, as indicated in the lower plot of Fig. 11.4. This is the condition for minimum OPD in the presence of fifth-order spherical. Then the shift of the reference point is given by   3 4LA z indicating that the best focus is three-fourths of the way from the paraxial focus to the zonal focus. The residual OPD is given by nLA z sin2 Um OPDm  OPDx   24

(11.13)

This is one-eighth of the OPD at the paraxial focus. Equating this to one-quarter wavelength, we find that the Rayleigh criterion allows a residual zonal spherical of 6 LA z   n sin2 Um

(11.14a)

To make an approximate conversion to transverse aberration, we multiply by sin Uz, which is approximately equal to 0.7 sin Um, and we get 4.2 4.2 TAz     NA n sin Um

(11.14b)

The Wave Aberration Polynomial

Equations 3.1 and 3.2 presented a power series expansion which expressed the transverse ray aberration as a function of h, s, and  (see Fig. 3.1 for the meaning of these terms.) A similar expression can be derived for the wave-front aberration, or OPD.

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355

OPD  A′1s2  A′2sh cos   B′1s4  B′2s3h cos   B′3 s2h2 cos2   B′4 s2h2  B′5 sh3 cos   C′1s6  C′2s5h cos   C′4 s4h2  C′5 s4h2 cos2   C′7 s3h3 cos   C′8 s3h3 cos3   C′10 s2h4  C′11 s2h4 cos2   C′12 sh5 cos   D′1 s8  . . . Note that although the constants here correspond to those in Eqs. 3.1 and 3.2, they are not numerically the same. However, the expressions are related by l ∂OPD y′  TAy    n ∂y

and

l ∂OPD x′  TAx    n ∂x

where l is the pupil-to-image distance and n is the image space index. Note that the exponent of the semiaperture term s is larger by one in the wave-front expression than in the ray-intercept equations. This equation allows us to determine the shape of the wave front for any combination of aberrations. 11.4 Aberration Tolerances The preceding sections form a basis for the establishment of what are usually referred to as aberration tolerances. We should note, however, that the use of the word “tolerance” in this connection does not carry the same go, no-go connotation that it does in matters mechanical, where parts may suddenly cease to fit or function when tolerances are exceeded. Any amount of aberration degrades the image; a larger amount simply degrades it more. Thus, it might be more accurate to call this section “Aberration Allowances.” The Rayleigh criterion, or limit, allows not more than one-quarter wavelength of OPD over the wave front with respect to a reference sphere about a selected image point in order that the image may be “sensibly” perfect. For convenience, we will use the term one Rayleigh limit to mean an OPD of one-quarter wavelength. We have previously noted that the image formed by a perfect lens is a diffraction pattern which contains 84 percent of its energy in a central disk, the remaining 16 percent being distributed in the rings of the pattern. When the OPD is less than several Rayleigh limits, the size of the central disk is basically unchanged, but a noticeable shift of energy from the central disk to the rings takes place. RMS OPD

The preceding discussions have measured the OPD in terms of its maximum departure from the reference sphere. This is often referred

356

Chapter Eleven

to as peak-to-peak or peak-to-valley (P-V) OPD. It correlates well to image quality when the shape of the wave front is relatively smooth. However, it is inadequate if the wave front is abruptly irregular. In such circumstances the RMS OPD is a better measure of the effect of the wave-front deformation. RMS stands for “root mean square,” and is the square root of the average (or mean) of the squares of all the OPD values sampled over the full aperture of the system. Consider, for example, an otherwise perfect optical system with a bump on one surface. If the bump covers only a very small area, its effect on the image will be correspondingly small, even if the P-V OPD of the bump in the wave front is quite large. In this sort of case the RMS OPD would be very small and would represent the effect of the bump on the image much more accurately than the P-V OPD would. The relationship between RMS OPD and P-V OPD for the case of the very smooth wavefront deformation caused by defocusing is P-V OPD RMS OPD   3.5 For a less smooth wave-front deformation the denominator in this expression will be larger; this is especially true for deformations caused by high-order aberrations or by fabrication errors. Most workers assume a denominator of 4 or 5 in the above expression when dealing with random errors. Thus the Rayleigh quarter-wave criterion corresponds to an RMS OPD of a fourteenth- or a twentieth-wave. The fact that a twentieth-wave sounds much more impressive than a quarter-wave may have contributed to the popularity of RMS OPD among suppliers of optical systems. Strehl Ratio

The Strehl ratio is the illumination at the center of the Airy disk for an aberrated system expressed as a fraction of the corresponding illumination for a perfect system, as shown in Fig. 11.5. It is a good measure of image quality when the optical system is well corrected. A Strehl ratio of 80 percent corresponds to a quarter-wave P-V OPD (exactly for defocus, approximately for most aberrations.) For modest amounts of OPD, the relationship between the Strehl ratio and the RMS OPD is well approximated by 2

Strehl ratio  e (2)

where  is the RMS OPD in waves. For various amounts of OPD, the several measures of image quality are related as indicated in the following table. It assumes that the OPD is due to defocusing. The P-V OPD is given in both Rayleigh lim-

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357

Figure 11.5

Relation of Image Quality Measures to OPD

% energy in

P-V OPD

RMS OPD

Strehl ratio

Airy disk

Rings

0.0 0.25RL  /16 0.5RL  /8 1.0RL  /4 2.0RL  /2 3.0RL  0.75 4.0RL

0.0 0.018 0.036 0.07 0.14 0.21 0.29

1.00 0.99 0.95 0.80 0.4* 0.1* 0.0*

84 83 80 68 40 20 10

16 17 20 32 60 80 90

*The smaller values of the Strehl ratio do not correlate well with image quality.

its (RL) and wavelengths. The Marechal criterion for image quality is a Strehl ratio of 0.80, which corresponds to the Rayleigh limit for defocusing but is otherwise more general than the quarter-wave limit. Thus it is apparent that an amount of aberration corresponding to one Rayleigh limit does cause a small but appreciable change in the characteristics of the image. For most systems, however, one may assume that, if the aberrations are reduced to the Rayleigh limit, the performance will be first class and that it will take a determined investigator a considerable amount of effort to detect the resultant difference in a performance. An occasional system does require correction to a fraction of the

358

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Rayleigh limit. Microscopes and telescopes are usually corrected to meet or better the Rayleigh criterion, on the axis at least; photographic lenses approach this level of correction only infrequently. The following tabulation indicates the amount of aberration corresponding to one Rayleigh limit (OPD  /4) when the reference point is chosen to minimize the P-V OPD. Out of Focus Longitudinal:

l′   (11.15) 2n sin2 Um Transverse: 0.5 H′   NA Third-Order Marginal Spherical Longitudinal: 4 (11.16) LAm   n sin2 Um Transverse: 4 TAm   NA Zonal Residual Spherical (LAm  0) Longitudinal: 6 LAz   n sin2 Um

(11.17)

Transverse: 4.2 TAz   NA Tangential Coma 1.5 ComaT   NA

(11.18)

Chromatic aberration Axial color: LAch  L′F  L′C   n sin2 Um TAch   NA

(11.19)

Lateral color: 0.5 TchA  H′F  H′C   NA

(11.20)

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359

The symbols are , the wavelength of light; n, the index of the medium in which the image is formed; Um, the slope angle of the marginal axial ray at the axial image; H, the image height; NA  n sin Um, the numerical aperture. The allowance for longitudinal color is derived from the out-of-focus allowance; if the reference point is midway between the long- and short-wavelength focal points, it is apparent that they may be separated by twice the out-of-focus allowance before the Rayleigh limit is exceeded. For the chromatic aberrations these amounts are less significant in terms of their effect on the image quality (e.g., MTF) than are the quarter-wave amounts of the monochromatic aberrations. This is because only the extreme wavelengths (e.g., C and F) are a quarterwave off the nominal wage front; all the other wavelengths are at less than a quarter-wave. Since for most systems the spectral response is at least somewhat peaked up for the central wavelengths, this means that for chromatic aberrations in amounts corresponding to Eqs. 11.19 and 11.20, more than half of the effective illumination has less than an eighth-wave OPD. Thus for ordinary chromatic one can assume that 1.8 to 2.5 (depending on whether the system spectral response is flat or peaked) times the amounts indicated above will produce about the same effect on the image as the quarter-wave amounts for the monochromatic aberrations. If the chromatic is in the form of secondary spectrum, factors of 2.5 to 4.5 are appropriate. Note that the human visual response is quite peaked and factors approaching the larger ones above are suitable for visual systems. The allowance for coma is frequently exceeded, since it is extremely difficult to correct a system to this level of quality over an appreciable field. The out-of-focus allowance is, of course, applicable to curvature of field, and values of zs and zt (xs and xt) should (ideally, at least) be less than twice this amount. However, it is a rare system that can be corrected to this level, and most optical systems which cover an extended field exceed this allowance many times over. Example A

For a visual optical system with a relative aperture of f/5, sin Um  0.10 and  0.55 m  0.00055 mm. The aberration allowances corresponding to one-quarter wave OPD are thus given by: 0.00055 Out of focus  ±  2 (0.1)2

 ±0.0275 mm

4 (0.00055) Marginal spherical  ±   ±0.22 mm (0.1)2

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6 (0.00055) Zonal spherical  ±   ±0.33 mm (LAm  0) (0.1)2 1.5 (0.00055) Tangential coma  ±   ±0.00825 mm 0.1 0.00055 Axial chromatic  ±   ±0.055 mm ( ±0.13 mm realistically) (0.1)2 11.5 Image Energy Distribution (Geometric) When the aberrations exceed the Rayleigh limit by several times, diffraction effects become relatively insignificant, and the results of geometric raytracing may be used to predict the appearance of a point image with a fair degree of accuracy. This can be done by dividing the entrance pupil of the optical system into a large number of equal areas and tracing a ray from the object point through the center of each of the small areas. The intersection of each ray with the selected image plane is plotted, and since each ray represents the same fraction of the total energy in the image, the density of the points in the plot is a measure of the power density (irradiance, illuminance) in the image. Obviously the more rays that are traced, the more accurate the representation of the geometrical image becomes. A ray intercept plot of this type is called a spot diagram. Figure 11.6 indicates several methods of placing the rays in the entrance pupil and shows an example of a spot diagram. The rectangular ray placement is the most used, being the easiest to do and also having utility in OPD and MTF calculations. The preparation of a spot diagram obviously entails a great amount of raytracing. As pointed out in Section 10.4, the rays on each side of the meridional plane are mirror images of each other; this reduces the necessary raytracing by 50 percent. The number of rays to be traced can be reduced markedly by an interpolation process. To produce a spot diagram which faithfully reproduces the image, several hundred ray intersections are required. However, if 20 or 30 rays are traced, it is possible to fit an interpolation equation to their intercept coordinates so that the required (larger) number of points can be computed from the equation. Equations such as Eqs. 3.1 and 3.2 are suitable for this purpose. However, the high computation speed now available in most desktop computers makes this unnecessary, and most spot diagrams are made by simply tracing several hundred rays through the system. For an accurate analysis, the effects of wavelength on the energy distribution must also be included. This is accomplished by tracing additional rays at different wavelengths; the variation of system

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The upper sketches show the placement of rays in the entrance pupil so that each ray “represents” an equal area. Shown below are a spot diagram (for a system with pure coma) and the line spread functions (below and to the right) obtained by counting the number of points between parallel lines separated by a small distance, Y or Z.

Figure 11.6

sensitivity with wavelength may be taken into account by tracing fewer rays in the less-sensitive wavelengths or by an appropriate weighting scheme. For devices with appreciable fields of view, spot diagrams must also be prepared for several obliquities. Focusing must also be taken into account. Since it is difficult to predict in advance the exact position of the plane of best focus, spot diagrams are often prepared for several positions of the image plane and the best is selected. One way of accomplishing this is to hold the final ray data (intercepts and directions) in the computer memory and to calculate a new set of intercepts for each focus shift. 11.6 Spread Functions—Point and Line The image of a point (whether the data are derived from a spot diagram or from an exact diffraction calculation) can be considered from a three-dimensional point of view to be a sort of illumination

362

Chapter Eleven

mountain, as sketched in Fig. 11.7. The point spread function can be described two dimensionally by a series of cross sections through the three-dimensional solid. The solid corresponding to a line image is also shown in Fig. 11.7. The cross section of the line solid is called the line spread function and can be obtained by integrating the point solid along sections parallel to the direction of the line, since the line image is simply the summation of an infinite number of point images along its length. The lower part of Fig. 11.6 shows a spot diagram for a system with pure third-order coma and the line spread functions derived from it. A knife-edge trace is a plot of the energy which passes a knife edge versus the position of the knife edge as the knife is scanned laterally through the image of a point. The slope, or derivative, of the knife-edge scan is equal to the value of the line spread function. This relationship is often used to measure the line spread function in order to measure the MTF (see Sec. 11.8). 11.7 Geometric Spot Size Due to Spherical Aberration

Third-order spherical aberration

The meridional spread of an image can, of course, be read directly from a ray intercept curve (see Fig. 3.24, for example). For points on the axis, the image blur is symmetrical and it is possible to obtain simple expressions for the size of the blur spot. Figure 11.8 shows the ray paths near the image plane of a system afflicted with third-order spherical aberration. It is apparent that the minimum diameter blur spot for this system occurs at a point between the marginal focus and the paraxial focus. This point is three-quarters

The energy distribution in the image of a point (a) and a line (b). The line image (b) is generated by summing an infinite number of point images (a) along its length. The line spread function is the cross section of (b). Figure 11.7

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The upper figure shows the ray paths near the focus of a system with thirdorder spherical aberration. The smallest blur spot occurs at 0.75LAm from the paraxial focus. The lower figure is a ray intercept curve (H′ vs. tan U′) for the same case; the slope of the dashed lines (dH′/d tan U′) equals 0.75LAm and their separation indicates the diameter of the blur spot.

Figure 11.8

of the way from the paraxial focus to the marginal focus, and the diameter of the spot at this point is given by: B  1 2LA m tan Um  1 2TA m

(11.21)

Fifth-order spherical aberration

When the spherical aberration consists of both third and fifth orders, the situation is more complex. From a geometric standpoint, the minimum spot size can be shown to occur when the marginal spherical is equal to two-thirds of the (0.707) zonal spherical, or

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LAz  1.5LAm and LA  zero at y  1.12Ym. For most systems, this means that both LAm and LAz are undercorrected when the minimum geometric spot size is desired. Then the “best” focus occurs at   1.25LAm  0.83LAz and the size of the blur spot is B  1 2LA m tan Um  1 3LA z tan Um

(11.22)

However, if the marginal spherical is corrected to zero, then the “best” geometric focus is at   0.42LA z and for small values of U, the minimum blur spot size is B  0.84LA z tan Um

(11.23)

The “best” focus positions described above are not necessarily those one would select visually, and the reader may have noticed that they differ from those selected on the basis of OPD in Sec. 11.3. Figure 11.9 shows a ray intercept curve for fifth-order spherical with the marginal spherical corrected to zero. The slope of the two solid lines indicates the amount of focus shift required to minimize the blur spot. (Remember that the slope H/ tan U is equivalent to a focus shift, and that the vertical separation of the lines indicates the size of the blur.) However, the dashed pair of lines (which enclose the ray intercepts from about 80 percent of the aperture) indicate a focus position at which there is a much higher concentration of light within a much smaller spot, and this is usually the preferred focus, even though the total spread of the image is greater by a factor of almost 2. The concept of minimum blur size is little used in optical systems for visual or photographic work, since the minimum geometric blur position is seldom, if ever, chosen as the focus. However, in systems which use photodetectors, one frequently wishes to determine the smallest detector that will collect all the energy in the image. Under such circumstances, the blur spot sizes given by Eqs. 11.21, 11.22, and 11.23 are extremely useful; in Chap. 13, a number of very convenient equations are presented which make use of this concept to predict the performance of several simple optical systems which are frequently used in conjunction with photodetectors. The geometric spot minimum is

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The image blur spot size for third- and fifth-order spherical aberration, balanced for LAm  0, illustrating the effects of various focus settings. Figure 11.9

often a consideration when a system’s performance is well below that of a “diffraction-limited” system. Example B

A visual system, working at f/5 (sin Um  0.1), which has an undercorrected third-order longitudinal spherical aberration of 0.22 mm, will have its minimum diameter blur spot 0.75  0.22  0.165 mm ahead of the paraxial focus, and by Eq. 11.21 the size of this blur spot will be equal to B  1 2  0.22  0.1005  0.011 mm It is interesting to note that on the basis of the OPD analysis, the best focus should occur 0.5  0.22  0.11 mm ahead of the paraxial focus and that the diameter of the central disk of the Airy pattern is equal to 1.22 1.22 (0.00055)     0.0066 mm n sin U 0.1 This central disk should contain about 68 percent of the energy in the image, since a marginal spherical of 0.22 mm is equal to just one Rayleigh limit (as shown in Example A). If an f/5 system has third- and fifth-order spherical with a corrected marginal and a zonal residual of 0.33 mm (again in longitudinal measure), the smallest geometric spot size would be found at about 0.42  0.33  0.14 mm from the paraxial focus and the spot size would be B  0.84  0.33  0.1005  0.028 mm Here the comparison with the OPD analysis is less fortuitous. The zonal spherical of 0.33 mm is again equivalent to one Rayleigh limit; we would expect the central disk of the diffraction pattern to be 0.0066

366

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mm as above, and the best focus to be about 0.75  0.33  0.25 mm from the paraxial focus. The agreement with geometry is somewhat better if we use the focus indicated by the dashed lines of Fig. 11.9; the position of “best focus” is almost exactly the same as the OPD best focus and the diameter of the intense center spot of the geometric pattern is to the order of 0.01 mm. 11.8

The Modulation Transfer Function

A type of target commonly used to test the performance of an optical system consists of a series of alternating light and dark bars of equal width, as indicated in Fig. 11.10a. Several sets of patterns of different spacings are usually imaged by the system under test and the finest set in which the line structure can be discerned is considered to be the limit of resolution of the system, which is expressed as a certain number of lines per millimeter.* When a pattern of this sort is imaged by an optical system, each geometric line (i.e., of infinitesimal width) in the object is imaged as a blurred line, whose cross section is the line spread function. Figure 11.10b indicates a cross section of the brightness of the bar object, and Fig. 11.10c shows how the image spread function “rounds off” the “corners” of the image. In Fig. 11.10d, the effect of the image blur on progressively finer patterns is indicated. It is apparent that when the illumination contrast in the image is less than the smallest amount that the system (e.g., the eye, film, or photodetector) can detect, the pattern can no longer be “resolved.” If we express the contrast in the image as a “modulation,” given by the equation max.  min. Modulation   max.  min. (where max. and min. are the image illumination levels as indicated in Fig. 11.10d), we can plot the modulation as a function of the number of lines per millimeter in the image, as indicated in Fig. 11.11a. The intersection of the modulation function line with a line representing the smallest amount of modulation which the system sensor can detect will give the limiting resolution of the system. The curve indicating the smallest amount of modulation detectable by a system or sensor (i.e., the threshold) is often called an AIM curve, where the initials stand for the aerial image modulation required to produce a response in the sys-

*Note that in optical work the convention is to consider a “line” to consist of one light bar and one dark bar, i.e., one cycle. In television parlance, both light and dark lines are counted. Thus, 10 “optical” lines indicate 10 light and 10 dark lines, whereas 10 “television” lines indicate 5 light and 5 dark lines. To avoid confusion, “optical” lines are frequently referred to as line pairs, e.g., 10 line pairs per millimeter.

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The imagery of a bar target. (a) A typical bar target used in testing optical systems consists of alternating light and dark bars. If the pattern has a frequency of N lines per millimeter, then it has a period of 1/N millimeters, as indicated. (b) A plot of the brightness of (a) is a square wave. (c) When an image is formed, each point is imaged as a blur, with an illumination distribution described by the spread function. The image then consists of the summation of all the spread functions. (d) As the test pattern is made finer, the contrast between the light and dark areas of the image is reduced. Figure 11.10

tem or sensor. The response characteristics of the eye, films, image tubes, CCDs, etc., are appropriately described by an AIM curve. Note that the modulation threshold usually rises with spatial frequency, although there are exceptions. Figure 5.4 is effectively an AIM curve for the eye; note that at very low angular frequencies the contrast threshold of the eye rises (for physiologic reasons). It should be apparent that the limiting resolution does not fully describe the performance of the system. Figure 11.11b shows two modulation plots with the same limiting resolution, but with quite different performances. The plot with the greater modulation at the lower frequencies is obviously superior, since it will produce crisper, more

368

Chapter Eleven

(a) The image modulation can be be plotted as a function of the frequency of the test pattern. When the modulation drops below the minimum that can be detected, the target is not resolved. (b) The system represented by (a) will produce a superior image, although both (a) and (b) have the same limiting resolution.

Figure 11.11

contrasty images. Unfortunately, the type of choice one is usually faced with in deciding between two systems is less obvious. Consider Fig. 11.11c, where one system shows high limiting resolution and the other shows high contrast at low target frequencies. In cases of this type, the decision must be based on the relative importance of contrast versus resolution in the function of the system.* The preceding discussion has been based on patterns whose brightness distribution is a “square wave” (Fig. 11.10b) and whose image illumination distribution is distorted or “rounded off” by characteristics of the optical system, as indicated in Fig. 11.10d. However, if the object pattern brightness distribution is in the form of a sine wave, the distribution in the image is also described by a sine wave, regardless of the shape of the spread function. This fact has led to the widespread use of the modulation transfer function to describe the performance of a lens system. The modulation transfer function is the ratio of the *The Strehl definition is the ratio of the light intensity at the peak of the diffraction pattern of an aberrated image to that at the peak of an aberration-free image, and is one of the many criteria that have been proposed for image evaluation. It can be computed by calculating the volume under the (three-dimensional) modulation transfer function and dividing by the volume under the curve for an aberration-free lens (Sec. 11.10). A similar criterion for quick general evaluation of image quality is the normalized area under the modulation transfer curve.

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modulation in the image to that in the object as a function of the frequency (cycles per unit of length) of the sine-wave pattern. Mi MTF (v)   Mo A plot of MTF against frequency v is thus an almost universally applicable measure of the performance of an image-forming system and has been applied not only to lenses but to films, phosphors, image tubes, the eye, and even to complete systems such as camera-carrying aircraft. One particular advantage of the MTF is that it can be cascaded by simply multiplying the MTFs of two or more components to obtain the MTF of the combination. For example, if a camera lens with an MTF of 0.5 at 20 cycles per millimeter is used with a film with an MTF of 0.7 at this frequency, the combination will have an MTF of 0.5  0.7  0.35. If the object to be photographed with this camera has a contrast (modulation) of 0.1, then the image modulation is 0.1  0.35  0.035, close to the limit of visual detection. One should note, however, that MTFs do not cascade between optical components which are directly coherently “connected,” i.e., lenses which are not separated by a diffuser of some sort. This is because the aberrations of one component may compensate for the aberrations in another, and thus produce an image quality for the combination which is superior to that of either component. Any “corrected” optical system illustrates this point. In the past, the MTF has been referred to as frequency response, sine wave response, or contrast transfer function. If we assume an object consisting of alternating light and dark bands, the brightness (luminance, radiance) of which varies according to a cosine (or sine) function, as indicated by the upper part of Fig. 11.12, the distribution of brightness can be expressed mathematically as G (x)  b0  b1 cos (2 vx)

(11.24)

where v is the frequency of the brightness variation in cycles per unit length, (b0  b1) is the maximum brightness, (b0  b1) is the minimum brightness, and x is the spatial coordinate perpendicular to the bands. The modulation of this pattern is then (b0  b1)  (b0  b1) b M0    1 (b0  b1)  (b0  b1) b0

(11.25)

When this line pattern is imaged by an optical system, each point in the object will be imaged as a blur. The energy distribution within this blur will depend on the relative aperture of the system and the aberrations present. Since we are dealing with a linear object, the image of

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Chapter Eleven

Convolution of the object brightness distribution function G(x) with the line spread function A(). (a) The object function, G(x)  b0  b1 cos (2vx), plotted against x. (b) The line spread function A(). Note the asymmetry. (c) Illustrating the manner in which G(x) is modified by A(). A point (or more accurately, a line element) at x0 is imaged by the system as G(x0) times A(). Similarly at x0  1, the image of the line element is described by A()G(x0  1). Thus the image function at a given x has a value equal to the summation of the contributions from all the points whose spread-out images reach x. (d) The image function F(x)  ∫A()G(x  ) d has been shifted by  and has a modulation Mi  M0|A(v)|. Figure 11.12

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each line element can be described by the line spread function (Sec. 11.5, Fig. 11.7) indicated in Fig. 11.12 as A(). We now assume (for convenience) that the dimensions x and (1/v) in Eq. 11.24 are the corresponding dimensions in the image. It is apparent that the image energy distribution at a position x is the summation of the product of G(x) and A() and can be expressed as F(x)  ∫ A() G (x) d

(11.26)

Combining Eqs. 11.24 and 11.26, we get F(x)  b0∫ A() d  b1 ∫ A() cos [2v (x) ] d

(11.27)

After normalizing by dividing by ∫ A() d, Eq. 11.27 can be transformed to F(x)  b0  b1 |A(v)| cos (2vx)  b0  b1 Ac(v) cos (2vx)  b1 As(v) sin (2vx)

(11.28)

where |A(v)|  [A c2(v)  A s2(v) ]1/2

(11.29)

and

∫ A() cos (2v) d Ac(v)   ∫ A() d ∫ A() sin (2v) d As(v)   ∫ A() d

(11.30) (11.31)

Ac(v) cos    |A(v)|

(11.32)

As(v) tan    Ac(v)

(11.33)

Note that the resulting image energy distribution F(x) is still modulated by a cosine function of the same frequency v, demonstrating that a cosine distribution object is always imaged as a cosine distribution image. If the line spread function A() is asymmetrical, a phase shift  is introduced. This is a lateral shift of the location of the image (at this frequency). The modulation in the image is given by b1 (11.34) Mi   |A(v)|  M0 |A(v)| b0 and |A(v)| is the modulation transfer function.

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Chapter Eleven

Mi MTF(v)  |A(v)|   M0 The optical transfer function (OTF) is the complex function which describes this process. It is a function of the spatial frequency v of the sine-wave pattern. The real part of the OTF is the modulation transfer function (MTF) and the imaginary part is the phase transfer function (PTF). If the PTF is linear with frequency, it is, of course, just a simple lateral displacement of the image (as, for example, distortion), but if it is nonlinear, it can have an effect on the image quality. A phase shift of 180° is a reversal of contrast, in that the image pattern is light where it should be dark, and vice versa. See Fig. 15.24 for example. 11.9 Computation of the Modulation Transfer Function We will illustrate the computation of the MTF by a grossly simplified and abbreviated example. In actual practice, a much larger number of points must be used in the computation if accurate results are to be obtained. We assume that a spot diagram has been prepared from raytrace data as shown in Fig. 11.13a. The line spread function is determined by integrating the spot diagram in one direction; in practice, one assumes an increment x and counts all the spots between the lines bounding the increment. A normalized plot of Nx against x then represents the line spread function A(x). (Note that the point spread function could be derived from a diffraction calculation if the diffraction MTF were desired.) Since real spread functions are rarely (if ever) represented by ordinary analytic functions, we cannot use Eqs. 11.30 and 11.31 in their integral form. A close approximation (which lends itself nicely to electronic computer usage) is given by the equivalent summation equations, ∑A(x) cos (2vx) x Ac(v)   ∑A(x) x ∑A(x) sin (2vx) x As(v)   ∑A(x) x

(11.35) (11.36)

As a numerical example, we will determine the value of the MTF for a frequency of v  0.1, i.e., one-tenth cycle per unit length. The values of A(x), the line spread function, which we will use are given in line 2 of Fig. 11.14 for various values of x. Line 4 of the table gives the values of 2vx for these same values of x, and Lines 5 and 6 give the values of cos (2vx) and sin (2vx) for each point.

Image Evaluation

The calculation of the modulation transfer factor for a given frequency, v. (a) The spot diagram is summed in one direction by counting the number of spots (ray intersections) in each increment, x. (b) The number of spots is plotted against x to get the line spread function A(x). A(x) is usually normalized to peak at unity. (c) A(x) cos (2vx) and A(x) sin (2vx) are generated by point-for-point multiplication of A(x) by the trigonometric functions. Then ∫A(x) cos (2vx) dx and ∫A(x) sin (2vx) dx are the areas under their respective curves (remembering that area below the x-axis is negative). Similarly ∫A(x) dx is the area under the curve of A(x) vs. x. These values are used in Eqs. 11.29 through 11.34 to get the MTF and phase shift  for the frequency v. Figure 11.13

373

374

Figure 11.14 Numerical computation of the modulation transfer function for a frequency of v  0.1 cycles per millimeter, from the line spread function (x) given in line 2.

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Now Lines 7 and 8 give A(x) cos (2vx) and A(x) sin (2vx), respectively. Since x is equal to 1.0 in this example, we can obtain the required summations for Eqs. 11.35 and 11.36 by summing across lines 2, 7, and 8, giving us 冱A(x) x  5.10 冱A(x) cos (2vx) x  2.51236 冱A(x) sin (2vx) x  0.0 Note that the last value is a foregone conclusion when A(x) is a symmetrical function of x, since the positive and negative values of the sine function on either side of x  0 cause one side to cancel the other when summed. Thus, when A(x) is symmetrical, the labor of the calculation can be reduced by a factor of 4, since only one-half of the cosine function needs to be evaluated. Inserting the above values into Eqs. 11.35 and 11.36, we find that 2.51236 Ac(0.1)    0.4926 5.1 0.0 As(0.1)    0.0 5.1 and that by Eqs. 11.29 and 11.33 MTF(0.1)  |A(0.1)|  (0.4932  02)1/2  0.493 0 tan     0.0 2.512 Thus, for a frequency v  0.1 cycles per unit length, we find a modulation transfer factor of 49 percent. This calculation can be repeated for several values of v, and a plot of the MTF against frequency, similar in appearance to those of Fig. 11.11, can be prepared from the results. As mentioned above, a much smaller value of x must be used if accurate results are to be obtained. Square-wave vs. sine-wave targets

Once the MTF has been determined (plotted) for a range of frequencies, it is possible to determine an analogous function for the modulation transfer of a square wave pattern, i.e., a bar target of the type shown in Fig. 11.10. This is done by resolving the square wave into its Fourier components and taking the sine wave response to each component. Thus, for a given frequency v, the square wave modulation transfer S(v) is given by the following equation [in which MTF(v) is written M(v) for clarity].

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Chapter Eleven

M(3v) M(5v) M(7v) 4 S(v)   M(v)        . . . 3 5 7  The inverse of this function is

冤

冥

冤

冥

 S(7v) S(3v) S(5v) M(v)   S(v)       . . . 4 3 5 7

(11.37a)

(11.37b)

Practicle resolution considerations

A rough indication of the practical meaning of resolution can be gained from the following, which lists the resolution required to photograph printed or typewritten copy. Excellent reproduction (reproduces serifs, etc.) requires 8 resolution line pairs per the height of a lowercase letter e. Legible (easily) reproduction requires 5 line pairs per letter height. Decipherable (e, c, o partly closed) requires 3 line pairs per letter height. Point sizes of type (where P is the point size) are Height of an upper case letter  0.22P mm  0.0085P in Height of a lower case letter  0.15P mm  0.006P in The correlation between resolution in cycles per minimum dimension (height, length of military targets) and certain functions (often referred to as Johnson’s law) is Detect

1.0 line pairs per dimension

Orient

1.4 line pairs per dimension

Aim

2.5 line pairs per dimension

Recognize

4.0 line pairs per dimension

Identify

6–8 line pairs per dimension

Recognize with 50% accuracy

7.5 line pairs per height

Recognize with 90% accuracy

12. line pairs per height

11.10 Special Modulation Transfer Functions: Diffraction-Limited Systems Section 11.9 discussed MTF in geometric terms; the spot-diagram techniques set forth there are applicable only when the aberrations are large. When they are small, the interactions between the diffraction

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effects of the system aperture and the aberrations become very complex. If there are no aberrations present, the MTF of a system is related to the size of the diffraction pattern (which is a function of the numerical aperture of the system and the wavelength of the light used). For a “perfect” optical system, the MTF is 2 MTF(v)   (  cos  sin ) (11.38)  where v   cos1  2NA

冢

冣

and v is the frequency in cycles per millimeter, is the wavelength in millimeters, NA is the numerical aperture (n′ sin U′), and cos1 (x) means the angle whose cosine is x.* It is apparent that MTF(v) is equal to zero when  is zero; thus, the “limiting resolution” for an aberration-free system, often called the cutoff frequency, is 1 2NA v0     (f/#)

(11.39)

where is in millimeters, f/# is the relative aperture of the system, and v0 is in cycles per millimeter. Notice that an optical system is a lowpass filter which cannot transmit information at a higher spatial frequency than the cutoff frequency v0. For an afocal system (or one with the image at infinity), the cutoff frequency is given by v0  D/ cycles/radian A plot of Eq. 11.38 is shown in Fig. 11.15; the frequency scale is in terms of v0, the limiting frequency given by Eq. 11.39. It should be noted that for ordinary systems, this level of performance cannot be exceeded. A geometric MTF curve derived from the raytrace data (and neglecting diffraction) of a well-corrected lens will sometimes exceed the values of Fig. 11.15; such results are, of course, incorrect and derive from the fact that the light ray concept only partially describes

*Equation 11.38 applies to uniformly illuminated and transmitting circular apertures. For apertures of any other shape, the diffraction MTF is equal to the (normalized) area common to the aperture and the aperture displaced. Equation 11.38 is thus the (normalized) area common to two circles of radius R, as their centers are separated by an amount equal to 2vR/v0. For a rectangular aperture the plot of MTF would thus be a straight line. The cutoff frequency v0 is computed from Eq. 11.39 in each case using the aperture size (i.e., the f/# or NA) in the direction of the resolution.

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The modulation transfer function of an aberrationfree system (solid line). Note that frequency is expressed as a fraction of the cutoff frequency. The dashed line is the modulation factor for a square wave (bar) target. Both curves are based on diffraction effects and assume a system with a uniformly transmitting circular aperture.

Figure 11.15

The effect of defocusing on the modulation transfer function of an aberration-free system.

Figure 11.16

(a) In focus

OPD  0.0 sin2

(b) Defocus

 /(2n

(c) Defocus

 /(n sin2 U)

OPD  /2

(d) Defocus

 3 /(2n sin2 U)

OPD  3 /4

(e) Defocus

 2 /(n sin2 U)

OPD 

(f) Defocus

 4 /(n sin2 U)

OPD  2

U)

OPD  /4

(Curves are based on diffraction effects—not on a geometric calculation.)

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the behavior of electromagnetic radiation. Note also that aberrations always reduce the MTF. The effects of small amounts of defocusing on the diffractionlimited MTF are shown in Fig. 11.16. Note that curve B corresponds to the depth of focus allowed by one Rayleigh limit as discussed in Secs. 11.2 and 11.4. The small effect produced by an OPD of onequarter wavelength indicates the astuteness of Rayleigh’s selection of this amount as one which would not “sensibly” affect the image quality. By way of comparison, Fig. 11.17 shows the MTF plots which would be obtained by geometrical calculations of a perfect system defocused by the same amounts. The agreement between Fig. 11.16, whose curves are derived from wave-front analysis, and Fig. 11.17 is poor for small amounts of OPD. However, when the defocusing is sufficient to introduce an OPD of one wavelength or more, the agreement becomes much better. Note that all the curves of Fig. 11.17 are of the same family and that one can be derived from another by a simple ratioing of the frequency scale. These curves are representations of 2J1(Bv) J1(2NAv)  MTF(v)   ≈ Bv NAv

(11.40)

where J1( ) indicates the first-order Bessel function,* B is the diameter of the blur spot produced by defocusing,  is the longitudinal defocusing, NA is the numerical aperture, and v is the frequency in cycles per unit length. Note that in Figs. 11.16 and 11.17, some of the curves show a negative value for the MTF. This indicates that the phase shift in the image ( in Eq. 11.33) is 180° and that the image is light where it should be dark and vice versa. This is known as spurious resolution (since a line pattern can be seen, but it is not a true image of the object) and is a phenomenon which is frequently observed in defocused, well-corrected lenses or in lenses whose defocused image of a point is a nearly uniformly illuminated circular blur. See Fig. 15.24 for example. In Fig. 11.18, the effects of third-order spherical aberration on MTF are shown. Note once again that the effect of an amount of aberration corresponding to the Rayleigh limit (OPD  /4) is quite modest. The situation here is quite similar to the defocusing case, in that MTF curves based on geometrical calculations are in poor agreement with Fig. 11.18 where the aberration is small, but in quite reasonable

x

冱 k0

*Jn(x) 

(1)k xn2k  2(n2k) k!(n  k)!

(x/2)5 x (x/2)3 J1(x)        ... 2 122 12223

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The effect of defocusing on the geometrically calculated modulation transfer function of an aberration-free system. (a) In focus OPD  0.0 (b) Defocus  /(2n sin2 U) OPD  /4 (c) Defocus  /(n sin2 U) OPD  /2 (d) Defocus  2 /(n sin2 U) OPD  (e) Defocus  4 /(n sin2 U) OPD  2 These geometrically derived plots are in poor agreement with the exact diffraction plots of Fig. 11.16 when the defocusing is small. The agreement at OPD  (curve D above, curve E in Fig. 11.16 is fair; the match at OPD  2 is quite good).

Figure 11.17

agreement where the aberration is to the order of one or two wavelengths of OPD. Figure 11.19 shows the effect of a central obstruction in the aperture of a diffraction-limited system. Note that the introduction of a disk into the aperture* drops the response at low frequencies but raises it slightly at high frequencies (although it cannot change v0, the cutoff frequency). Thus, a system of this type tends to show greatly reduced contrast on coarse targets and a somewhat higher limit of resolution (when used with a system which requires a modulation of more than zero to detect resolution). This is the result of shifting light from the airy disk to the rings of the diffraction pattern. MTF with coherent and semi-coherent illumination

All the preceding discussions (except that dealing with a central obstruction of the aperture) have assumed a uniformly illuminated *Apodization is the use of a variable transmission filter or coating at the aperture to modify the diffraction pattern. Coatings which reduce the transmission at the center of the aperture tend to “favor” the response at high frequencies; coatings which reduce transmission at the edge of the aperture tend to favor the lower frequencies.

Image Evaluation

The effect of third-order spherical aberration on the modulation transfer function. (a) LAm  0.0 OPD  0 (b) LAm  4 /(n sin2 U) OPD  /4 (c) LAm  8 /(n sin2 U) OPD  /2 (d) LAm  16 /(n sin2 U) OPD  These curves are based on diffraction wave-front computations for an image plane midway between the marginal and paraxial foci. Figure 11.18

The effect of a central obscuration on the modulation transfer function of an aberration-free system.

Figure 11.19

(a) s0/sm  0.0 (b) s0/sm  0.25 (c) s0/sm  0.5 (d) s0/sm  0.75

381

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and uniformly transmitting aperture. When the illumination system is arranged so that only the central part of the aperture is illuminated (and this can be done with Koehler illumination if a projection condenser images the source at a size smaller than the pupil of the projection lens), then the MTF plot is modified in a way which is nearly the reverse of that shown in Fig. 11.19. Fourier theory tells us that we can consider the brightness distribution of an object to be the sum of many sinusoidal brightness distributions of differing frequencies, intensities, and orientations. To simplify matters, let us assume that we are projecting the image of a simple sinusoidal grating. Remembering that a sinusoidal grating has only the first diffraction order, consider the system shown in Fig. 11.20. If the illumination is coherent (i.e., collimated), the light from a point in the grating will be diffracted into the first order, as illustrated in Fig. 11.20a. If the angle of diffraction is less than that of the numerical aperture (NA) of the projection lens, the full power will be projected into the image. But if the grating frequency is high enough (so that v  NA/ ), the diffracted ray will pass outside the lens aperture, and no light corresponding to this frequency will make it into the image. The result of this situation is an MTF plot as shown in Fig. 11.20c, with 100 percent MTF for spatial frequencies of NA/ or less and zero MTF for all higher frequencies. Note that NA/ is just half the cutoff frequency (v0  2NA/ ), as given in Eq. 11.39 for the incoherent illumination case.

ILLUMINATED POINT

PUPIL DIFFRACTED RAY

MTF

COHERENT ILLUMINATION

(a) SINUSOIDAL GATING OBJECT

(b) OPTICAL SYSTEM

SEMICOHERENT ILLUMINATION

PUPIL

MTF

FREQUENCY (c)

2 NA

ILLUMINATED AREA OF PUPIL MTF MTF

DIFFRACTED CONE OF RAYS (d)

(e)

FREQUENCY (f)

2 NA

(a–c) The MTF with coherent illumination. (d–f) The MTF with semicoherent illumination (which partially fills the pupil). Figure 11.20

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If the illumination is semicoherent, the projection lens pupil will be partially filled, as indicated in Fig. 11.20d, e. As we consider an increasing grating frequency, the location of the illuminated area in the pupil will move toward the edge. However, at the edge of the pupil, the cutoff is gradual rather than abrupt, as in the coherent case described above, and we get an MTF plot of the sort shown in Fig. 11.20f. Figure 11.21 shows the effect on the MTF for several values of the illumination system NA, expressed as a fraction of the lens NA. These partial coherence effects are useful in both microlithography and microscopy. Note that decentering or tilting the illuminating beam can be used to get directional effects and that ring illumination can emphasize a particular frequency. As mentioned previously, MTFs have been applied to image-receiving systems which are not imaging systems. Figure 11.22 shows the MTF curves for a number of photographic emulsions. Since the MTF of a film is computed on the basis of equivalent relative exposures derived from density measurements on films exposed to sinusoidal test patterns, it is possible to have a film MTF greater than unity. This results from the chemical effects of development of the film on adjacent areas and will be noticed at the low-frequency end of the curves in Fig. 11.22. An AIM curve, as described in Section 11.8, can also be used to represent the response characteristics of nonimaging devices and sensors such as films. 11.11 Radial Energy Distribution The data of a point spread function or a spot diagram can be presented in the form of a radial energy distribution plot. If the blur spot is 100% COHERENT 0.37 0.5

INCOHERENT MTF

0.86

0.7

NA

2NA

FREQUENCY

MTF vs. frequency for a partially filled pupil (semicoherent illumination). Numbers are the ratio of illuminating system NA to optical system NA.

Figure 11.21

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Modulation transfer functions of several photographic emulsions.

Figure 11.22

symmetrical, it is apparent that a small circular aperture centered in the image would pass a portion of the total energy and block the rest. A larger aperture would pass a greater portion of the energy and so on. A graph of the encircled fraction of the energy plotted against the radius (semidiameter) of the aperture is called the radial energy distribution curve. A radial energy distribution curve, such as the example shown in Fig. 11.23, can be used to compute the MTF for an optical system by means of the summation equation MTF(v) 

im

冱

i1

Ei J0[2vR 苶i]

where v is the frequency in cycles per unit length, Ei is the difference (Ei  Ei1) between two values of E, the fractional energy, R 苶i is the average 1 2(Ri  Ri1) of the corresponding values of the radius and J0( ) indicates the zero-order Bessel function.* Although this radial energy distribution relationship is (strictly speaking) valid only for point images which have rotational symmetry, i.e., for images on the optical axis, it can be used to predict approximate averaged resolution for off-axis points. This procedure, while it cannot yield separate radial and tangential values for resolution, does serve to give the designer a rough idea of the state of correction of the system.

x 冣 冢2x冣 . . . 冢 2  4

冢 冣

x *sJ0(x)1  2

2

1222

6

122232

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385

Radial energy distribution plot. The curve indicates the fraction E of the total energy in an image pattern which falls within a circle of radius R. Thus all the energy is encompassed by a circle of radius Rm; Ei of the energy by a circle of radius Ri. Figure 11.23

11.12 Point Spread Functions for the Primary Aberrations The figures of this section illustrate the effects of the primary aberrations on the point spread function (PSF) of an optical system. Figures 11.24 through 11.28 each show four point spread functions, the first for a peak-to-valley OPD (wave-front deformation) of an eighth-wave, the second for a quarter-wave (which is the Rayleigh criterion), the third for a half-wave, and the fourth for a full wavelength of OPD. The caption for each figure also gives the rms (root mean square) OPD and the Strehl ratio for each PSF (see Sec. 11.4 and Fig. 11.5). Figure 11.24 shows the effect of simple defocusing on the PSF. Note that for defocusing, the Rayleigh criterion (which is the OPD equal to a quarter-wave) is identical to the Marechal criterion (Strehl ratio equal to 0.80). In Fig. 11.25, which shows the effect of simple thirdorder spherical aberration, the PSF for an eighth-wave is almost identical to that for defocusing, and the quarter-wave PSF is very similar. But when we compare the half- and full-wave plots, the differences are quite apparent, despite the fact that the effects on the MTF and resolution are still comparable. The coma PSF in Fig. 11.26, however, is noticeably different even at an OPD of an eighth-wave, where the unsymmetrical rings in the diffraction pattern are already apparent. At one wave of OPD the PSF is clearly showing the “comma-” or “comet-shaped” figure that one gets from a geometric optics spot diagram (see Fig. 11.6 for example). Figure 11.27 may be a bit surprising to some readers. Most discussions of astigmatism (including that in Sec. 3.2 of this text) which are based on geometric optics indicate that the blur spot between the sagittal and tangential focal lines is an ellipse or a circle, depending on where the image is examined. However, in the PSF for either half-

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Point spread functions for different amounts of defocus. (a) 0.125 wave (PV); 0.037 wave rms; 0.95 Strehl. (b) 0.25 wave (P-V); 0.074 wave rms; 0.80 Strehl. (c) 0.50 wave (P-V); 0.148 wave rms; 0.39 Strehl. (d) 1.00 wave (P-V); 0.297 wave rms; 0.00 Strehl. Figure 11.24

or full-wave OPD we can easily see that the blur spot is not circular but has a definite four-sided aspect. Anyone who has microscopically examined the image of a point source formed by a lens with astigmatism as its major aberration will have observed this (and probably has wondered where the square-shaped image blur came from). It may help to understand this phenomenon to realize that the two focal lines are effectively acting as apertures, and the diffraction effect of this is to introduce the cross-shaped illumination distribution. The most customary balance between third-order and fifth-order spherical aberration is with the aberration of the marginal ray corrected to zero. This state of correction produces the least peak-to-valley OPD (as demonstrated in Sec. 11.3). In Fig. 11.28, the eighth-wave PSF is not very different from that for pure third-order spherical, or even defocus, but at a quarter-wave one begins to notice that the rings are more pronounced than they are in Figs. 11.24 and 11.25. This effect

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Point spread functions for different amounts of third-order spherical aberration. (a) 0.125 wave (P-V); 0.040 wave rms; 0.94 Strehl. (b) 0.25 wave (P-V); 0.080 wave rms; 0.78 Strehl. (c) 0.50 wave (P-V); 0.159 wave rms; 0.37 Strehl. (d) 1.00 wave (P-V); 0.318 wave rms; 0.08 Strehl. Note: Reference sphere centered at 0.5LAm (midway between marginal and paraxial foci).

Figure 11.25

is quite noticeable in a star test, where heavy rings in the diffraction pattern are an indication of a zonal spherical residual. The final figure in this series, Fig. 11.29, compares the PSF for the various aberrations, each of which is set at a value which equals the Marechal criterion (a Strehl ratio of 80 percent). There are differences apparent if one looks very closely at the defocus and spherical plots, and there are obvious differences for astigmatism and coma. However, the net effect on the image quality is surprisingly similar. This is, of course, the reason that the Rayleigh criterion of a quarter-wave (peakto-valley) OPD and the Marechal criterion of 0.80 Strehl are so widely accepted by lens designers as a standard of image quality. Note: These figures were prepared by applying an optical software program to systems which were set up to show only the particular aberration under consideration. A paraboloidal reflector was the obvious choice for the defocusing PSF because its axial image is total-

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Point spread functions for different amounts of third-order coma. (a) 0.125 wave (P-V); 0.031 wave rms; 0.96 Strehl. (b) 0.25 wave (P-V); 0.061 wave rms; 0.86 Strehl. (c) 0.50 wave (P-V); 0.123 wave rms; 0.65 Strehl. (d) 1.00 wave (P-V); 0.25 wave rms; 0.18 Strehl. Note: P-V OPD reference sphere centered at 0.25ComaT from chief ray intersection point. rms OPD reference sphere centered at 0.226ComaT from chief ray intersection point.

Figure 11.26

ly aberration-free. The spherical aberration plots were created by deforming the paraboloid with a fourth-order deformation term for the third-order spherical plot and fourth- and sixth-order deformations for the third- and fifth-order spherical plot. The coma PSF was calculated using a paraboloidal reflector with its aperture stop at the focal plane (which eliminates astigmatism), as in Fig. 13.37a. The image was put on a curved surface which approximated a sphere of radius equal to the focal length of the reflector and which was centered at the center of curvature of the paraboloid. The astigmatism PSF was produced by introducing an additional cylindrical parabolic reflector. Bibliography Note: Titles preceded by an asterisk are out of print. Altman, J. H., “Photographic Films,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 20.

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Point spread functions for different amounts of astigmatism. (a) 0.125 wave (P-V); 0.026 wave rms; 0.97 Strehl. (b) 0.25 wave (P-V); 0.052 wave rms; 0.90 Strehl. (c) 0.50 wave (P-V); 0.104 wave rms; 0.65 Strehl. (d) 1.00 wave (P-V); 0.207 wave rms; 0.18 Strehl. Note: Reference sphere centered midway between sagittal and tangential foci.

Figure 11.27

Boreman, G. D., “Transfer Function Techniques,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 32. Born, M., and E. Wolf, Principles of Optics, New York, Pergammon Press, 1999. *Conrady, A., Applied Optics and Optical Design, Oxford, 1929. (This and vol. 2 were also published by Dover, New York.) Gaskill, J., Linear Systems, Fourier Transforms, and Optics, New York, Wiley, 1978. Goodman, J., Introduction to Fourier Optics, New York, McGraw-Hill, 1968. Herzberger, M., Modern Geometrical Optics, New York, Interscience, 1958. *Hopkins, M., Wave Theory of Optics, Oxford, 1950. Levi, L., and R. Austing, Applied Optics, vol. 7, Optical Society of America, Washington, 1968, pp. 967–974 (defocused MTF). *Linfoot, E., Fourier Methods in Optical Design, New York, Focal, 1964.

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Point spread functions for different amounts of zonal spherical aberration (third- and fifth-order spherical balanced so that marginal spherical equals zero). (a) 0.125 wave (P-V); 0.042 wave rms; 0.93 Strehl. (b) 0.25 wave (P-V); 0.085 wave rms; 0.75 Strehl. (c) 0.50 wave (P-V); 0.208 wave rms; 0.35 Strehl. (d) 1.00 wave (P-V); 0.403 wave rms; 0.09 Strehl. Note: Reference sphere centered at 0.75LAz for P-V and at 0.8LAz for rms. Figure 11.28

Marathay, A. S., “Diffraction,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 3. *O’Neill, E., Introduction to Statistical Optics, Reading, Mass., Addison-Wesley, 1963. Perrin, F., J. Soc. Motion Picture and Television Engrs., vol. 69, March–April 1960 (MTF, with extensive bibliography). Selwyn, E., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 2, New York, Academic, 1965 (lens-film combination). Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985. Suits, G., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985 (film).

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Point spread functions for five different aberrations, each with a Strehl ratio of 0.80 (the Marechal criterion). In each case the center of the reference sphere is located to minimize the rms OPD, which is 0.075 wave for all five aberrations. (a) Defocus: 0.25 wave (P-V). (b) Third-order spherical: 0.235 wave (P-V). (c) Balanced thirdand fifth-order spherical: 0.221 wave (P-V). (d) Astigmatism: 0.359 wave (P-V). (e) Coma: 0.305 wave (P-V).

Figure 11.29

Wetherell, W., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (calculation of image quality). Exercises 1 The longitudinal spherical aberration of a spherical reflector is equal to y2/8f (to a third-order approximation). What is the maximum diameter a 36-in focal-length spherical reflector may have without exceeding an OPD of onequarter wavelength for visual light,  20  10-6 in ? (use Eg. 11.16) answer: 4.7 in 2 The third-order sagittal coma of a parabolic reflector is given by y2/4f, where  is the half-field angle in radians. What is the maximum diameter a

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36-in focal-length sperical reflector cover without exceeding the Rayleigh limit? (  2  105 in) answer: ±0.0041 radians (0.47° total field) 3 An f/5 system is defocused by 0.05 mm. What is the modulation transfer factor for a “sine wave” target with a spatial frequency (at the image) of 120 cycles per millimeter? Use Fig. 11.16, Eq. 11.2, and assume  0.5 m. ANSWER:

0.23

Chapter

12 The Design of Optical Systems: General

12.1 Introduction In the immediately preceding chapters, we have been concerned with the analysis of optical systems, in the sense that the constructional parameters of the system were given and our object was the determination of the resultant performance characteristics. In this chapter we take up the synthesis of optical systems; here the desired performance is given and the constructional parameters are to be determined. A large part of the synthesis process is, of course, concerned with analysis, since optical design is in great measure a systematic application of the cut-and-try process. There is no “direct” method of optical design for original systems; that is, there is no sure procedure that will lead (without foreknowledge) from a set of performance specifications to a suitable design. However, when it is known that a certain type of design or configuration is capable of meeting a given performance level, it is a fairly straightforward process for a competent designer to produce a design of the required type. Further, modest improvements to existing designs can almost always be effected by well-established techniques. Thus, it is apparent that a good portion of the ammunition in a lens designer’s arsenal consists of an intimate and detailed knowledge of a wide range of designs, their characteristics, limitations, idiosyncrasies, and potentials. Here is one part of the art in optical design; basically it consists of the choice of the point at which the designer begins. 393

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The electronic computer, in the course of little more than a decade, radically modified the techniques used by optical designers. Previously a designer resorted to all manner of ingenious techniques to avoid tracing rays because of the great expenditure of time and effort involved. The computer has reduced raytracing time by many orders of magnitude, and it is now easier to trace rays through a system than it is to speculate, infer, or interpolate from incomplete data. A computer can even be made to carry through the entire design process from start to finish, more or less without human intervention. The results produced by such a process are nonetheless intricately dependent on the starting point elected (as well as the manner in which the computer has been programmed), so that a great deal of art (if perhaps somewhat less personal satisfaction) is still present in even the most automatic technique. The ordinary design process can be broken down into four stages, as follows: first, the selection of the type of design to be executed, i.e., the number and types of elements and their general configuration. Second, the determination of the powers, materials, thicknesses, and spacings of the elements. These are usually selected to control the chromatic aberrations and the Petzval curvature of the system, as well as the focal length (or magnifying power), working distances, field of view, and aperture. (Choices made at this stage may affect the performance of the final system tremendously, and can mean the difference between success and failure in many cases). In the third stage, the shapes of the elements or components are adjusted to correct the basic aberrations to the desired values. The fourth stage is the reduction of the residual aberrations to an acceptable level. If the choices exercised in the first three stages have been fortuitous, the fourth stage may be totally unnecessary. At the other extreme, the end result of the first three stages may be so hopeless that a fresh start from stage 1 is the only alternative. In fully automatic computer design procedures, a portion of stage 1 and all of stages 2, 3, and 4 may be accomplished more or less simultaneously (using an approach that might take a human computer a lifetime or two to slog through). Computer design techniques are discussed in Sec. 12.8. The basic principles of optical design will be illustrated by three detailed examples in the following sections. A simple meniscus (box) camera lens will be used to show the effects of bending and stop shift techniques, as well as the handling of a simplified exercise in satisfying more requirements than there are available degrees of freedom. An achromatic telescope objective will introduce material choice, achromatism, and multiple bending techniques. An air-spaced (Cooke) triplet anastigmat will illustrate the problem of controlling all the

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395

first- and third-order aberrations in a system with just a sufficient number of degrees of freedom to accomplish this and will further illustrate the technique of material selection. The design characteristics of several additional types of optical systems are discussed in Chaps. 13 and 14. At this point it should be emphasized that the design procedures implied by the discussions in Secs. 12.2, 12.4 to 12.6, and to some extent 12.7, while perfectly valid, are presented here as a way of explaining the principles, relationships, limitations, etc., involved in the design. These procedures are rarely used today; the computer, especially the desktop personal computer, or PC, has enough computing power so that every designer can have access to some sort of automatic lens design program. Nonetheless, a knowledge of these procedures and principles is of great utility to a designer, even when using an automatic design program. For example, such knowledge helps in selecting a good starting design for the computer and, among other things, often helps in figuring out what went wrong when the designer has asked the computer to do the optically impossible. 12.2

The Simple Meniscus Camera Lens

There are just two elements to work with in the design of a meniscus camera lens, the lens itself and the aperture stop. If, for the moment, we restrict ourselves to a thin, spherical-surfaced element, the parameters which we may choose or adjust are the material of the lens, its focal length, its shape (or bending), the position of the stop, and the diameter of the stop. With these degrees of freedom we must design a lens which will produce an acceptable image on a given size of film. This implies that all the aberrations of the system must be “sufficiently” small. It is immediately apparent that the spherical aberration will be undercorrected and that the Petzval curvature will be inward-curving (and equal to h2/2n); these are the immutable characteristics of a simple lens. Thus, the element power, the size of the aperture, and the field of view must be chosen small enough so that the effects of these aberrations are tolerable. The lens material usually chosen is common crown glass or acrylic plastic, on the basis of cost, since a box camera lens must be inexpensive. A high-index crown does not produce enough improvement in the Petzval curvature to warrant its increased cost; a flint glass would introduce increased chromatic aberrations. We find ourselves with just two uncommitted degrees of freedom, namely the bending of the lens and the position of the stop. Now in a simple undercorrected system it is axiomatic that for a given (i.e., fixed) shape of the lens (or lenses), the position of the stop (the “natural” stop

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position—see Sec. 3.4) for which the coma is zero is also the position for which the astigmatism is the most overcorrected (i.e., most backwardcurving). Since the Petzval surface will be inward (toward the lens) curving, some overcorrected astigmatism is desirable. Thus the design technique is straightforward: we choose (arbitrarily) a shape for the lens, determine the stop position at which coma is zero, and evaluate the aberrations. By repeating this process for several bendings and graphing the aberrations as a function of the shape, we can then choose the best design. There are several ways in which this can be accomplished. Since this is a simple lens of moderate aperture and field, the third-order aberrations are quite representative of the system and one would be quite safe in relying on them. The design could also be handled by trigonometric raytracing. For this example we will work out the design using the thin-lens (G-sum) third-order aberration equations and then check the results by raytracing. Assuming that the glass has an index of 1.50 and a V-value of 62.5, we will set up the G-sum equations for a focal length of 10, an aperture diameter of 1.0, and an image height of 3 (all in arbitrary units and all subject to scaling and adjustment later). Thus, the element power   1 ⁄10  0.1, and the total curvature c  c1  c2  /(n  1)  0.2. With the object at infinity, #1  0. Using the G-values worked out in Example G of Chap. 10, we find that the spherical and coma (stop at the lens) given by Eqs. 10.8m and 10.8n are TSC  0.145833C12  0.05C10.005625 CC  0.0625C1  0.01125 Now the position of the stop can be determined by solving Eq. 10.8g for Q when CC* is zero. CC*  0  CC  Q TSC CC Q  TSC Equations 10.8o, p, and r give us TAC  0.0225 TPC  0.015 TAchC  0.008 and by substituting the above into Eqs. 10.8h, j, and l, we get the following expressions for the third-order astigmatism, distortion, and lateral color with the stop as defined by Q above.

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397

TAC*  0.0225  2Q CC  Q 2 TSC DC*  0.0825Q  3Q 2CC  Q 3TSC TchC*  0.008Q Having established the above relationships, we now select several values for C1 and evaluate the third-order aberrations for each. The results are indicated in the tabulation of Fig. 12.1 and the graph of Fig. 12.2. Note that Xs  PC*  AC* and Xt  PC*  3AC*. [Here we revert to the older symbol (X) for field curvature rather than the currently popular Z.] A study of Fig. 12.2 can be quite rewarding. First, we note that there are two regions which appear most promising, namely the meniscus shapes at either side of the graph. On the left, the lens is concave to the incident light and (since Q is positive) the stop is in front of the lens. To the right the lens is convex to the incident light and the stop is behind the lens. Both forms have more undercorrected spherical aberration than the less strongly bent shapes, but both have their field curvature “artificially” flattened by overcorrected astigmatism. Note that the form with the least spherical aberration (where CC  0 and the stop is in contact with the lens) has the most strongly inward curving field. This inward-curving field is characteristic of any thin optical system with the stop in contact, since by Eqs. 10.8p and 10.8h h2 (3n  1) Stop in contact X T  PC*  3AC*   2n

Figure 12.1 Tabulation of the third-order aberrations of a thin lens with the stop at the

coma-free position, for various values of C1.

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Figure 12.2 The third-order ab-

errations of a thin lens (f  10, y  0.5, h  3, n  1.5) with the stop at the coma-free position, plotted as a function of the curvature of the first surface (C1).

Selecting the bending C1  0.2 for further investigation, we note that Q  1.11 (from Fig. 12.1). Since Q  yp/y and y  0.5, we find yp  0.555. The slope of the principal ray in object space which will yield an image height h  3 with a focal length of 10 is up  0.3. The stop position is thus yp 0.555 lp      1.85 up 0.3 or 1.85 units to the left of the lens. We must of course convert our thin lens to a real lens. A ray with a slope of 0.3 through the upper edge of the stop (diameter  1.0) will strike the lens at a height of 1.05, and we shall assume a diameter of twice this for the lens. We determine the curvature of the second

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399

surface from C2  C1  C  0.2  0.2  0.4, and compute the sagittal heights of the surfaces for the diameter of 2.10. Thus for our lens to have an edge thickness of 0.1, it must have a center thickness of CT  ET  SH 1  SH 2  0.1  0.11  0.23  0.22. We now trace an oblique fan of four equally spaced meridional rays through the system and calculate two values of coma (by Eq. 10.6d), one from the upper three rays and one from the lower three. By linear interpolation between the two overlapping three ray bundles, we find that a bundle with a chief ray axial intercept of L pr   1.664 will have zero coma. This is the stop position for the thick lens (vs. l pr  1.85 for the thin lens.) The results of a raytrace analysis are shown in Fig. 12.3. The field curvature and spherical aberration forecast by the thin-lens thirdorder computations are shown as circled points, and the agreement with the actual raytrace is quite good. Note that complete TOA plots could be derived from our knowledge of the manner in which the TOA vary with aperture and image height (see the tabulation of Fig. 3.16). For example, knowing that (longitudinal) third-order spherical varies as Y2 and that SC  0.429 for Y  0.5, we could determine that SC  0.107 for Y  0.25 and plot it accordingly. In Fig. 12.3 the dashed lines in the ray intercept plots indicate the portions of the ray fan which are intercepted by the stop.

Figure 12.3 The aberrations of a rear meniscus camera lens. The

circled points indicate the aberrations predicted by the thin-lens third-order aberration equations (G-sums).

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To complete the design we would next scale the entire system to the actual focal length desired. (Note that all the linear dimensions of any system, including the aberrations, may be multiplied by the same constant to effect a change in scale. No additional computation is necessary.) Next an appropriate size for the aperture would be selected, i.e., one which would reduce the aberration blurs to sizes commensurate with the intended application. The lens form that we have elected to design in this example has the aperture stop in front, i.e., to the left of the lens. This is often referred to as the rear-meniscus form. From Fig. 12.2 it is apparent that there is a similar front-meniscus form with the stop behind (to the right of) the lens. Question: Which is the better design? On the basis of aberration correction, the rear meniscus is slightly better. However, there are several points on which the front meniscus is superior. In a camera, the length of the camera will be approximately equal to the lens focal length for the front meniscus, whereas for the rear meniscus we must add the distance to the stop, resulting in a significantly longer camera. Further, in an inexpensive camera, the shutter is usually a simple spring-driven blade located at the aperture stop. Thus, for the rear meniscus, the shutter mechanism is exposed to the environment; in the front meniscus, the lens acts as a protective window. Finally, and perhaps most important, in the front meniscus, the lens is out in front and quite visible to the customer, whereas in the rear meniscus, all the customer ever sees is the less appealing shutter mechanism. These latter “commercial” reasons are why the front-meniscus form has been universally used for inexpensive cameras since the 1940s. Apparently there is more to optical engineering than aberration correction. At the start of this section we assumed that the lens would be thin and its surfaces spherical. If we increase the thickness of a meniscus lens and maintain its focal length at a constant value by adjusting one of the radii, it is apparent from the thick-lens focal-length equation (Eq. 2.28) that we must either reduce the power of the convex surface or increase the power of the concave surface to maintain the focal length as the thickness is increased. Either change will have the effect of reducing the inward Petzval curvature of field. This principle (i.e., separation of positive and negative surfaces, elements, or components in order to reduce the Petzval sum) is a powerful one and is the basis of all anastigmat designs. The value of aspheric surfaces is limited in a design as simple as the box camera lens. However, if the lens is molded from plastic, an aspheric surface is as easy to produce as a spherical one; many simple cameras now have aspheric plastic objectives. The aspheric surface affords the designer additional freedom to modify the system to advantage. A

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diffractive surface could be used to achromatize the lens (and affect the other aberrations as well). 12.3

The Symmetrical Principle

In an optical system which is completely symmetrical, coma, distortion, and lateral color are identically zero. To have complete symmetry a system must operate at unit magnification and the elements behind the stop must be mirror images of those ahead of the stop. This is a principle of great utility, not only for systems working at unit power, but even for systems working at infinite conjugates. This is due to the fact that, although coma, distortion, and lateral color are not completely eliminated under these conditions, they tend to be drastically reduced when the elements of any system are made symmetrical, or even approximately so. For this reason many lenses which cover an appreciable field with low distortion and low coma tend to be generally symmetrical in construction. If we were to apply this principle to the meniscus camera lens, we would simply use two identical menisci equidistant on either side of the stop. The resulting lens would be practically free of coma, distortion, and lateral color. The periscopic lens, shown in Fig. 12.4, makes use of this principle. Symmetry, plus the thick meniscus principle (to flatten the field) achieves a very remarkable astigmatic field coverage of ±67° for the Hypergon lens, which is also shown in Fig. 12.4. This is accomplished at the expense of a heavily undercorrected spherical aberration which limits its useful speed to about f/30 or f/20.

12.4 Symmetrical (simple) meniscus lenses. The upper sketch shows a periscopic-type lens composed of two identical meniscus lenses. The lower sketch shows the Hypergon (U.S. Patent 706,650-1902), whose nearly concentric construction allows it to cover a total field of 135° at f/30. The inner and outer radii of the Hypergon differ by only one-half percent, producing a very flat Petzval curvature. Aberrations shown are for a focal length of 100.

Figure

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12.4 Achromatic Telescope Objectives (Thin-Lens Theory) An achromatic doublet is composed of two elements, a positive crown glass element and a negative flint glass element. (Stated more generally, an achromatic doublet consists of a low-relative-dispersion element of the same sign power as the doublet and a high-relativedispersion element of opposite sign.) As degrees of freedom we have the choice of glass types for the elements, the powers of the two elements, and the shapes of the two elements. We assume here that we are designing a telescope objective, that the stop or pupil will be located at the lens, and that the lens will be thin. The astigmatism of a thin lens in contact with the stop is fixed, regardless of the number of elements, their index, or their shapes. Equation 10.8o indicates TAC  (h 2u ′k )/2 for a single element. Since the power of a doublet is simply the sum of the powers of the elements, this equation applies to a doublet as well as a singlet. Thus we cannot affect the astigmatism (and can do very little about the Petzval curvature). The field will be strongly inward-curving. With reference to Fig. 12.5, it is apparent that we have only four variable parameters with which to correct the aberrations. Actually, one parameter must always be assigned to control the focal length in any lens design. Thus we have three variables left; we will use them to correct spherical aberration, coma, and axial chromatic aberration. Since the lens is to be free of chromatic aberration, we must assign the element powers to the determination of focal length and the control of chromatic aberration. Again we begin by using the thin-lens third-order aberration equations; assigning the subscripts a and b to the two elements, Eq. 10.8r gives us Ya2a Yb2 b  ∑TAchC  TAchC a  TAchC b  V u′   a k Vbu′k Since the elements are to be cemented together or very nearly in contact, we can substitute ya  yb  y and u′k  y/f to get

Figure 12.5 Achromatic doublet.

The Design of Optical Systems: General

b a ∑TAchC  fy    Va Vb

冤

冥

403

(12.1)

We now set ∑TAchC  0 (or some other value, if desired) and make a simultaneous solution of Eq. 12.1 with 1   a  b f

(12.2)

to get the necessary powers for the elements. For zero chromatic, we get Va a   f(Va  Vb)

(12.3)

aVb Vb b     Va f(Vb  Va)

(12.4)

Having determined a and b , we can now write thin-lens equations for the third-order spherical and coma in terms of the shapes of the elements [after tracing a marginal (thin-lens) paraxial ray to determine the values for u′k of the combination and # (or #′) for each element]. Since the aperture stop will be at the lens, Q  0.0 and the coma will be given by Eq. 10.8n. After the appropriate substitutions for h, y, Ca  a /(na  1), Cb   b /(n b  1), and the G-factors, we arrive at an equation of the following general form for coma: ∑CC  CCa  CCb  K1C1  K 2  K 3 C3  K 4  K1C1  K 3 C 3  (K 2  K 4)

(12.5)

where C1 and C3 are the curvatures of the first surfaces of the elements (Fig. 12.5), and K1 through K4 are constants. (Note that by using the alternate form of Eq. 10.8n for element a, the equation could be written in C2 and C3, the curvatures of the adjacent inner surfaces). Now for any desired value of ∑CC, we find that ∑CC  K1C1  K 2  K 4 C3   K3 or, combining constants C3  K 5 C 1  K 6

(12.6)

Thus for any shape of element a, Eq. 12.6 indicates the unique shape for element b which will give the desired amount of coma.

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In similar fashion we can write an expression for the thin-lens thirdorder spherical (using Eq. 10.8m) in the following form: ∑TSC  TSCa  TSCb  K7C12  K8C1  K9  K10C32  K11C3  K12 (12.7) By substituting the value for C3 from Eq. 12.6 into 12.7, and combining constants, we get a simple quadratic equation in C1 of the form 0  C12  K13C1  K14

(12.8)

which can be solved for the value of C1. When used with the value of C3 given by Eq. 12.6, this will yield a doublet with spherical and coma of the desired amounts. (Note that because Eq. 12.8 is a quadratic, there may be one, two, or no solutions.) For a first try, one would use the above procedure with ∑TAchC, ∑TSC, and ∑CC equal to zero (or whatever values are desired). Next, appropriate thicknesses are inserted, and the system tested by raytracing to determine the actual values of spherical, coma (or OSC), and axial color. If these are not within tolerable limits, the thin-lens solution can be repeated using (for the desired ∑TAchC, ∑TSC, and ∑CC) the negatives of the corresponding values determined by raytracing. This process converges to a solution very rapidly. While the above procedure is useful in understanding the nature of the doublet telescope objective, a designer with an optical software computer program could handle this project very easily. The four surface curvatures would be declared as variables, and the merit function would consist of targets for the actual ray-traced values of marginal spherical aberration, coma, and chromatic aberration plus the effective focal length. Given a reasonable starting lens form, the task is trivial, and the nearest solution to the starting form is found immediately. 12.5 Achromatic Telescope Objectives (Design Forms) Depending on the choice of glass, the relative aperture, the desired values of the aberrations, and also on which solution to the quadratic was selected, the procedure outlined in Sec. 12.4 will result in an objective with one of the forms sketched in Fig. 12.6. In general the edge contact form and, for lenses of modest (up to 3- or 4-in) diameter, the cemented form is preferred, primarily because the relationship between the elements (as regards mutual concentricity about the axis and freedom from tilt) can be more accurately maintained in fabrication. The crown-in-front forms are more commonly used because the

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Figure 12.6 Various forms of achromatic doublets. The

upper row are crown-in-front doublets and the lower row are flint-in-front. The curvatures are exaggerated for clarity. The center contact form is usually avoided because it is more difficult to manufacture. The shapes indicated are for lenses corrected for a distant object to the left.

front element is more frequently exposed to the rigors of weather; crown glasses are in general more resistant to weathering than flint glasses. The Fraunhofer and Steinheil forms represent one root of the quadratic of Eq. 12.8, and the Gauss form is the other root. Whether one gets the Fraunhofer or the Steinheil form simply depends on whether the left-hand element is of crown or flint glass. From an image-quality standpoint, there is little difference between them. However the Gauss objective is very different. The Gauss lens has about an orderof-magnitude more zonal spherical aberration residual and slightly (about 20 percent) more secondary spectrum than the Fraunhofer. However, it has only about half the spherochromatism. Another difference is that there is no solution for the Gauss form if the lens elements are too thick; thus the speed is limited to about f/5 or f/7 to avoid thick elements. The Fraunhofer and Steinheil forms can be corrected at speeds faster than f/3 (although the residual aberrations are of course quite large at high speeds). If one followed the procedure of Section 12.4, a design resulting in a cemented doublet (i.e., C2  C3) would be a lucky accident. When a cemented interface is necessary, an alternate procedure is followed. The spherical and coma contribution equations are written in C2 and C3 (instead of C1 and C3) and C2 is set equal to C3, resulting in

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equations in C2 (or C3) which may then be solved for either the desired coma or spherical. If these equations are plotted as a function of the shape of the doublet (i.e., versus C1 or C2 or C4) the resulting graph will look like one of those in Fig. 12.7, in which ∑TSC is a parabola and ∑CC is a straight line. In the left plot there is no solution for spherical, in the center plot the solutions for spherical and coma occur at the same bending, and on the right there are two possible solutions for spherical with equal and opposite-signed amounts of coma, and often with pronounced meniscus shapes. (These latter solutions are valuable if one desires to utilize the doublets in a symmetrical combination about a central stop, e.g., as an erector or a rapid rectilinear photo lens; the coma can then be used to reduce or overcorrect the astigmatism per Eq. 10.8h.) The exact form obtained is dependent primarily on the types of glass chosen. In general, the spherical aberration parabola can be raised by selecting a new flint glass with a lower index and higher V-value, or by selecting a new crown with a higher index and lower V. Thus the strongly meniscus solutions of the right-hand plot in Fig. 12.7 result from a glass pair with a small difference in V-value. Results approximating those in the middle graph of Fig. 12.7 can be obtained with BK7 (517:642) and SF2 (648:339). The best glass choice depends on the aperture (f/#) of the lens. Figure 12.8 shows the spherical aberration and the spherochromatism of a typical cemented doublet. As previously noted, the field curvature of a thin system with stop in contact is strongly inward and cannot be modified unless the stop is shifted. Thus, systems of this type are limited to applications which require good imagery over relatively small fields (a few degrees from the axis). It is occasionally desirable to produce a doublet objective with both the zonal and marginal spherical simultaneously corrected. This can be accomplished by using the airspace of a broken contact doublet as an added degree of freedom. The design is begun exactly as in Sec. 12.4, except that two (or more) thick-lens solutions are derived, one

Figure 12.7 The variation of spherical aberration (solid line) and coma

(dashed) as a function of the shape of a cemented achromatic doublet. Depending on the materials used there may be two forms with zero spherical (right), one form (center), or no form (left). The center graph is the preferred type since spherical and coma are both corrected.

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407

Figure 12.8 The spherical aberration and spherochromatism of a cemented

achromatic doublet, efl  100, f/3.0. Note that the chromatic is corrected at the margin. This is good practice if the spherochromatism is large; otherwise the image shows a blue flare. For small amounts, correction at the 0.7 zone is often a better choice.

with a minimum airspace and the other(s) with an increased space. The calculated zonal spherical is then plotted against the size of the airspace, and the airspace with LAz equal to zero is selected; this form will usually have no zonal OSC. Speeds of f/6 or f/7 can be attained with practically no spherical or axial coma over the entire aperture. Good glass choices are a light barium crown combined with either a dense flint or an extradense flint; either crown-in-front or flint-in-front forms are possible. In this type of lens the residual axial aberration consists almost solely of secondary spectrum. Spherochromatism, which is the variation of spherical aberration as a function of wavelength, can be corrected by a change in the spacing between elements (or components) which differ in the sign of their contributions to spherical and chromatic aberration. This general principle may be applied to the doublet achromat in a manner paralleling the use of the airspace to correct zonal spherical; indeed, the basic principle is the same for both aberrations. The source of spherochromatism can be understood by realizing that (in a cemented doublet) the two outer surfaces contribute under corrected spherical aberration, while the cemented interface contributes overcorrected spherical. The amount of the contribution varies directly

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with the size of the index change, or “break,” across the surface. The contributions are in balance for the nominal wavelength. At a shorter wavelength all the indices are higher; because of its greater dispersion, the index of the negative (flint) element increases about twice as rapidly as that of the positive (crown) element. The index break at all three surfaces is larger at the shorter wavelength. However, the index break at the outer surfaces is (n  1), whereas at the cemented surface it is (n′  n); as the wavelength and the indices change, (n′  n) changes proportionately more than does (n 1). Thus as we go to a shorter wavelength, the overcorrecting contribution of the cemented surface is increased more than the undercorrection from the outer surfaces. The result is that the short-wavelength light is overcorrected compared to the central or longer wavelength. This is spherochromatism. Now, if the airspace between elements is increased, as indicated in Fig. 12.9, the blue marginal ray, having been refracted more strongly than the red ray by the crown element, will strike the flint element at a lower height than will the red ray. Thus the refraction of the blue ray at the flint will be lessened relative to the red, and its overcorrection reduced accordingly. A very similar argument can be applied to the reduction of an undercorrected zonal spherical (which is caused by an overcorrected fifthorder spherical) by use of an increased airspace. The increased airspace affects the zonal spherical because the undercorrected spherical of the positive element bends the marginal ray toward the axis disproportionately more than the zonal ray. Thus, when the airspace is increased, the ray height at the overcorrecting negative element is reduced proportionately more for the marginal ray than for the zonal ray. The result is that the overcorrection is reduced more at the margin than at the zone, and, when the element shapes are readjusted to correct the marginal aberration, the zonal spherical is reduced. An airspaced doublet with reduced spherochromatism and reduced zonal spherical is shown in Fig.

Figure 12.9 The ordinary spherochromatism of a doublet can be corrected

by increasing the airspace [shown highly exaggerated in (b)]. This reduces the height at which the blue ray strikes the flint by a greater amount than for the red ray, thus reducing the overcorrection of the marginal blue ray. Sketches (c) and (d) show triplet forms which can be used to correct spherochromatism and spherical zonal residuals simultaneously.

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Figure 12.10 The spherical aberration and spherochromatism of an airspaced

achromatic doublet, efl  100, f/3.0. The size of the airspace used here is a compromise between the value which would minimize the zonal spherical aberration and that which would minimize the spherochromatism. Compare the residual aberrations with those of the cemented doublet in Fig. 12.8.

12.10. Both principles are applicable to more complex lenses as well. Figure 12.10 shows an example of these principles. One method of effecting a simultaneous elimination of both spherochromatism and zonal spherical is indicated in Fig. 12.9c. The doublet plus singlet configuration (in any of several arrangements of the elements) introduces still another degree of freedom, namely the balance of positive (crown) power between the two components, which can be used with the airspace to bring about the correction. The airspaced triplet shown in 12.9d is also capable of very good correction, but is more difficult to manufacture. Figure 13.53 illustrates the reduction of spherical by element splitting. Figure 14.3 shows an airspaced triplet telescope objective. The secondary spectrum (SS) contribution of a thin lens is given by Eq. 10.8t; combining this with the requirements for achromatism (Eqs. 12.3 and 12.4), we find that the secondary spectrum of a thin achromatic doublet is given by f P f (PbPa) SS    

V (VaVb)

(12.9)

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For any of the ordinary glass combinations used in doublets, the ratio P/ V is essentially constant, and the visual secondary spectrum is about 0.0004 to 0.0005 of the focal length. Similarly, the secondary spectrum of any achromatized combination of two separated components can be shown to be

P SS   [f 2  B (L2f ) ] D V

(12.10)

where D is the airspace, B the back focus, and L  B  D is the length from front component to the focal point. Again it is apparent that the ratio P/ V is the governing factor. Note that in this case the secondary color of two spaced positive lenses is less than that of a thin doublet of the same focal length; conversely, the secondary color of a telephoto lens (positive front component, negative rear component) or reversed telephoto is greater than the corresponding thin doublet. There are a few glasses which will reduce the secondary spectrum, for example, FK51, 52, or 54 used with a KzFS glass or an LaK glass as the flint element will reduce the visual secondary spectrum to a small fraction of the ordinary value. Note, however, that for most of these pairs Va  Vb is small, and the powers of the individual elements required for achromatism are higher than with an ordinary pair of glasses. This increase in element power causes a corresponding increase in the other residual aberrations. These glasses, with unusual partial dispersions, generally work poorly in the shop, lack chemical stability, and cannot withstand severe thermal shock. As mentioned in Chap. 7, calcium fluoride (CaF2, fluorite) may be combined with an ordinary glass (selected so that Pa  Pb) to make an achromat that is essentially free of secondary spectrum. It is also worth noting that there are no ordinary glass pairs which will form a useful achromat in the 1.0- to 1.5-m spectral band; fluorite can be combined with a suitable glass to make an achromat for this region. Silicon and germanium are useful for achromats at longer wavelengths, as are BaF2, CaF2, ZnS, ZnSe, and AMTIR. A triplet achromat can be used to reduce the secondary spectrum without the necessity of exactly matching the partial dispersions as in the doublet. If one plots the partial dispersion P against the V-value, most glasses fall along a straight line. What is needed to correct secondary spectrum is a pair of glasses with the same partial P, but with a significant difference in V-value. It turns out that in this sort of plot one can synthesize a glass anywhere along a line connecting two glass points by making a doublet of the two glasses. Thus one can arrange a triplet so that two of the elements synthesize a glass with exactly the same partial as the third glass. Some useful Schott glass combinations are (PK51, LaF21, SF15), (FK6, KzFS1, SF15), (PK51, LaSFN18,

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SF57); the power arrangement for these combinations is plus, minus, and weak plus, respectively. Other glass manufacturers have equivalent glass combinations. The thin lens element powers for a triplet apochromat can be found from the following equations, which are for a unit power (f  1.0) system. Define: X  Va (Pb  Pc)  Vb (Pc  Pa)  Vc (Pa  Pb) Then: a  Va (Pb  Pc) /X b  Vb (Pc  Pa) /X c  Vc (Pa  Pb) /X  1.0  a  b See Fig. 14.2 for an example of an apochromatic triplet telescope objective. A lens in which three wavelengths are brought to a common focus is called an apochromat. Often this term also implies that the spherical aberration is corrected for two wavelengths as well. By properly balancing the glass combinations given above one can achromatize the triplet for four wavelengths; such lenses are called superachromats.* Airspaced achromat (dialyte)

A widely airspaced doublet can be made achromatic, but the chromatic correction will vary with the object distance; it will be achromatic only for the design distance. The following equations will yield a separated achromatic doublet which is corrected for an object at infinity. VA B A   f (VAB  VBf ) VBf B   B (VAB  VBf ) (1  B/f ) D   A where f is the focal length, D is the airspace, and B is the back focal length.

*See M. Herzberger and N. McClure, “The Design of Superachromatic Lenses,” Applied Optics, vol. 2, June 1963, pp. 553–560.

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Athermalization

When the temperature of a lens element is changed, two factors affect its focus or focal length. As the temperature rises, all the dimensions of the element are increased; this, by itself, would lengthen the effective and back focal lengths. The index of refraction of the lens also changes with temperature. For many glasses the index rises with temperature; this effect tends to shorten the focal lengths. The change in the power of a thin element with temperature is given by d 1 dn      dt (n  1) dt

冤

冥

where dn/dt is the differential of index with temperature, and  is the thermal expansion coefficient for the lens material. Thus for a thin doublet d   ATA  BTB dt where 1 dn T    (n  1) dt and  is the doublet power. For an athermalized doublet (or for one with some desired d /dt), we can solve for the element powers

冤

冥

(d/dt)  TB A   TA  TB B    A To get an athermalized achromatic doublet, we can plot T against 1/V for all the glasses under consideration. Then a line drawn between two glass points is extended to intersect the T axis. The value of the d/dt for the achromatic doublet is equal to the doublet power times the value of T at which the extended line intersects the T axis. Thus one desires a pair of glasses with a large V-value difference and a small or zero T-axis intersection. An athermal achromatic triplet can be made with three glasses as follows: VA (TBVB  TCVC) A   D VB (TCVC  TAVA) B   D VC (TAVA  TBVB) C   D

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where D  VA (TBVB  TCVC)  VB (TCVC  TAVA)  VC (TAVA  TBVB), Vn is the V-value of element n, and T is defined above. 12.6

The Diffractive Surface in Lens Design

A diffractive surface as used in lens design is a fresnel surface (as shown in Fig. 9.15) “modulo 2.” In other words, it is a fresnel surface where the height of each step is such that the wave front is retarded or stepped by exactly one wavelength. Thus the step height is /(n  1), assuming that the surface is bounded by air. For a glass or plastic surface (n ≈ 1.5), this is a step height of about two wavelengths, as opposed to a step height on the order of tenths of a millimeter or more for an ordinary plastic fresnel. The slope and shape of the fresnel facets can be as defined by a sphere or an aspheric. Note that similar results can be obtained with a local variation of the index of refraction. Diffraction efficiency

The term kinoform indicates a surface with smooth facets. A curvedsurface kinoform theoretically can have 100 percent efficiency. A “linear” (cone-shaped) kinoform can be 99 percent efficient. A “binary” surface approximates the smooth fresnel facets with a stair-step contour produced by a high-resolution photolithographic process. The surface relief is created by exposure through a series of masks. The number of levels produced equals 2n, where n is the number of masks used, hence the name binary. The efficiency (i.e., the percentage of light which goes in the desired direction) of a binary surface is limited by the number of levels which are used to approximate the ideal smooth contour of the fresnel facet. A one-mask, 2-level surface is 40.5 percent efficient; a two-mask, 4-level surface is 81.1 percent efficient; a three-mask, 8-level surface is 95.0 percent efficient; a four-mask, 16-level surface is 98.7 percent efficient; and an M-level surface is [sin(/M)/(/M)]2 efficient. The theoretical efficiency of any diffraction surface, whether kinoform or binary, will be reduced by any fabrication departures from the ideal shape, such as rounding of sharp corners, etc. Since the wave front is stepped or retarded at each diffractive fresnel step by exactly one wavelength for the nominal wavelength, it is apparent that the coherent behavior of the system is preserved only for the nominal wavelength. At this wavelength, the phase from the top of one zone exactly matches that from the bottom of the preceding zone. The surface is less efficient for other wavelengths, and thus the spectral bandwidth over which a diffractive surface is useful is limited. This limitation may show up as inefficiency or as unwanted diffractive orders, ghosts, stray light, low contrast, etc. The efficiency at other than the nominal wavelength ( 0) is

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E  [sin  (1  0/ ) / (1  0/ ) ]2 Over a bandwidth of ( ), the average efficiency is ave E ≈ 1  [ ( ) /6 0]2

Manufacturability

The following expressions allow an estimate of the practicality or manufacturability of a diffractive lens. As indicated above, the step height is /(n  1). The radial spacing distance from one fresnel step to the next is approximately Spacing ≈ R /Y (n  1)  F /Y where R is the diffractive surface radius of curvature, F is its focal length, and Y is the radial distance from the axis. The minimum spacing (at the edge of the diffractive lens) is Min spacing ≈ 2 (f/#)  /NA where f/#  F/2Ymax  the relative aperture, and NA  n sin u  the numerical aperture. The total number of fresnel steps or zones is Number of steps ≈ D2/8 F where D is the lens diameter. It is apparent that the longer the wavelength and the weaker the power of the diffractive surface, the wider and deeper are the steps, and the easier is the fabrication task. Techniques used for fabrication include single-point diamond turning (especially good for long-wave IR), ion-beam machining, electron-beam writing, laser-beam writing, and photolithography (which is extremely difficult on curved surfaces but effective on plano surfaces). For large commercial quantities, injection-molded plastic elements are an economical choice. Another useful process is epoxy replication. Applications of diffractive optics include hybrid (combined refractive and diffractive) lenses, microlens (size about 50 m) arrays, anamorphic arrays, prisms, beamsplitters, beam multiplexers, filters, etc. The Sweatt model

From a lens design standpoint, an easy way to handle and understand the use of a diffractive surface is through the Sweatt model. W. C. Sweatt* showed that a raytrace model consisting of a very high index, *J. Opt. Soc. Am., vol. 67, 1977, p. 80; vol. 69, 1979, p. 486; Appl. Opt., vol. 17, 1978, p. 1220.

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415

zero-thickness lens could be used to predict the effect of a diffractive surface; the higher the index, the closer the results of the raytrace come to matching the exact diffraction results. An index of about 10,000 is a reasonable value to use. Since the diffractive effect is a direct function of wavelength, the index of the model should vary as the wavelength, and n ( )  1  (n0  1) ( / 0) where 0 and n0 are the nominal wavelength and index, respectively. Thus, for the visual region, using d, F, and C light, we have for d-light at 0.5875618 m, nd  10,001.00 F-light at 0.4861327 m, nF  8,274.73 C-light at 0.6562725 m, nC  11,170.42 and the Abbe V-value, V  (nd  1) / (nF  nC)  3.45 The negative V-value results from the fact that the index rises with wavelength instead of dropping as in ordinary refractive materials. The partial dispersion is P  (nF  nd)/(nF  nC)  0.5962. These extremely unusual values make the diffractive surface a most singular optical material. This low-V-value (i.e., high dispersion) characteristic of a diffractive device indicates that there will be very large amounts of chromatic aberration when a diffractive surface is used over a significant spectral bandwidth. The achromatic diffractive singlet

If we assume a single element of BK7 (nd  1.5168, V  64.2, P  0.6923), we can apply Eqs. 12.3 and 12.4 to determine the powers of the singlet and the diffractive element which will produce an achromat. The result is a power of a  Va/(Va  Vb)  0.949 for the BK7 element and b  0.051 for the diffractive element (where  is the desired power of the achromat). The negative V-value of the diffractive surface produces an achromat where both elements have positive power. If we allow the diffractive surface to be aspheric (in the actual surface this is done by making the slope and shape of the fresnel facets

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correspond to those of an aspheric surface), we can produce a singlet of the desired power which is corrected for spherical aberration, chromatic aberration, and coma. The necessary four degrees of freedom are the power and bending of the singlet and the power and fourth-order asphericity (or conic constant) of the diffractive surface. The resulting design is shown in Fig. 12.11. The residual aberrations (zonal spherical, spherochromatism, and secondary spectrum) can be compared with those of the ordinary achromatic doublet shown in Fig. 12.8. Note that the sign of the secondary spectrum is reversed from that of an ordinary doublet (because of the unusual P and V of the diffractive surface) and that the spherochromatism is large, more than twice that of the doublet of Fig. 12.8 (and is also of reversed sign). The spherochromatism can be corrected by aspherizing the first surface with a fourth-order deformation term in a manner analogous to adjusting the airspace of the doublet in Fig. 12.10 (i.e., we change the relative heights at which the red and blue rays strike the diffractive surface). The zonal spherical can be removed with a sixth-order deformation term on the first surface. The use of an aspheric surface is an

RADIUS

THICKNESS

MATERIAL

59.307733

4.50

BK7

1.5168

64.17

–972.261092

0.00

DIFF 10,001.

–3.45

–972.186542*

97.415

AIR

*Conic constant kappa = –0.186743

RED "C" LIGHT

YELLOW "d" LIGHT 15 BLUE "F" LIGHT 10

C -LIGHT d-LIGHT F-LIGHT

5 TRANSVERSE ABERRATION (RAY INTERCEPT PLOT)

0.04 0.03 0.02 0.01 0 –0.01 –0.02 –0.03 –0.04

–0.4 –0.3 –0.2–0.1 0 0.1 0.2 0.3 LONGITUDINAL ABERRATION

Figure 12.11 The spherical aberration and spherochromatism of a hybrid refractive-

diffractive singlet, efl  100, f/3.0. Compare with the doublet of Fig. 12.8 (but note that the scales for LA are different). Both the spherochromatism and secondary spectrum are larger and of the opposite sign from Fig. 12.8. As indicated in the text, the spherochromatism and the zonal spherical can be eliminated easily by aspherizing the first surface (which would be quite a feasible option if the lens were injection-molded from acrylic).

The Design of Optical Systems: General

417

economically practical move, assuming that the lens is to be injectionmolded from plastic. The result is a lens whose only axial aberration is about 0.17 mm of secondary spectrum. Alternately, because photolithographic fabrication is most conveniently done on a flat surface, one might want to limit the lens shape to a plano-convex form and use as degrees of freedom the lens index, its radius, the power of the diffractive surface, and its asphericity. The optimal index is about 1.55 for this lens. If the lens material is acrylic (n  1.492), and if we elect to control focal length, spherical, and chromatic (neglecting coma), the tangential coma at one degree off axis is 0.0156; if the material is polystyrene (n  1.590), it is 0.0101. Achromatic diffractive singlets have been very satisfactorily used in eyepieces, magnifiers, zoom camera lenses, and many other applications where the object field is of relatively uniform brightness. Their compactness and light weight as compared with a glass achromat make them very desirable for many applications such as head-mounted displays. Diffractive surfaces sometimes have proven less satisfactory for systems where there is a high brightness source in (or near) the field of view or a wide spectral bandwidth. The apochromatic diffractive doublet

Since the unusual V-value and partial dispersion of the diffractive surface are so far from the line of normal glasses in a P versus V plot, we can easily produce an apochromatic lens using two ordinary glasses plus a diffractive surface to eliminate the secondary spectrum. The element powers for a three-element apochromat can be found using the following equations: X  Va (Pb  Pc)  Vb (Pc  Pa)  Vc (Pa  Pb) a  Va (Pb  Pc) /X b  Vb (Pc  Pa) /X c  Vc (Pa  Pb) /X where  is the power of the apochromatic triplet, Vi is the V-value, and Pi is the partial dispersion of the ith element. If we use acrylic (n  1.4918, V  57.45, P  0.7014) and polystyrene (n  1.5905, V  30.87, P  0.7108) for elements a and b, and the diffractive surface (n  10,001, V  3.45, P  0.5962) for element c, we get the following starting powers for the elements: a  1.9544

(acrylic)

b  0.9640

(polystyrene)

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c  0.0096

(diffractive)

The lens can be corrected for marginal and zonal spherical aberration, coma, chromatic, spherochromatic, and secondary spectrum using the techniques outlined above. A drawback for this particular lens is that the secondary spectrum varies with aperture and is corrected only at one zone. 12.7 The Cooke Triplet Anastigmat The Cook triplet is composed of two outer positive crown elements and an inner flint element, with relatively large airspaces separating the elements. This type of lens is especially interesting because there are just enough available degrees of freedom to allow the designer to correct all of the primary aberrations. The basic principle used to flatten the field curvature (i.e., the Petzval sum) is quite simple: the contribution that an element makes to the power of a system is proportional to y, and the contribution to the chromatic varies with y2. However, the contribution to the Petzval curvature is a function of  alone and is independent of y. Now in a thin (compact) system, all the elements have essentially the same value of y and the powers of the elements are determined by the requirements of focal length and chromatic correction; consequently, the Petzval radius of a thin doublet is often about 1.4f, and rarely exceeds 1.5 or 2 times the focal length. However, when the negative elements of a system are spaced away from the positive elements (so that the ray height y at the negative elements is reduced), the power of the negative elements must be increased to maintain the focal length and chromatic correction of the system. As a result, the overcorrecting contribution of the negative element to the Petzval curvature is increased. Thus by the proper choice of spacing, the Petzval radius can be lengthened to several times the system focal length and the field proportionately “flattened.” From Fig. 12.12, which shows a schematic triplet, we can determine the available degrees of freedom. They are 1. Three powers (a, b, c) 2. Two spaces (S1, S2) 3. Three shapes (C1, C3, C5) 4. Glass choice 5. Thicknesses Of these, items 1, 2, and 3 will be of immediate interest; they total eight variables. Item 4, glass choice, is an extremely important tool, but we will reserve its discussion until later. Item 5, element thickness, is only

The Design of Optical Systems: General

419

Figure 12.12 The Cooke triplet

anastigmat.

marginally effective; in regard to the primary corrections, its effect duplicates that of the spacings. With these eight degrees of freedom, the designer wishes to correct (or control) the following primary characteristics and aberrations. 1. Focal length 2. Axial (longitudinal) chromatic aberration 3. Lateral chromatic aberration 4. Petzval curvature 5. Spherical aberration 6. Coma 7. Astigmatism 8. Distortion Thus, there are just the necessary eight degrees of freedom to control the eight primary corrections. Note that the fact that there are eight variable parameters does not guarantee that there is a solution. The relationships involved are, in several instances, nonlinear, as the thin-lens equations (Eqs. 10.8) indicate. It is entirely possible to choose a set of desired aberration values and/or glass types for which there is no solution. On the other hand, it is also possible that there are as many as eight solutions, as will be seen in the following paragraphs. Power and spacing solution. The first four items listed immediately

above can be seen (by reference to the thin-lens third-order aberration equations) to be functions of element power and ray height (which is a function of spacing); they are independent of element shape. Thus, it is necessary that the powers and spaces be chosen to satisfy these four conditions, which may be expressed as follows: Power: 1 1 Desired      ∑y f ya

(12.11)

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Chapter Twelve

Axial color: y2 1 Desired ∑TAchC   ∑  V u′k

(12.12)

yyp 1 Desired ∑TchC*   ∑  V u′k

(12.13)

 h2 Desired ∑PC   ∑  n 2

(12.14)

Lateral color:

Petzval sum:

where the summation is over the three elements. These expressions are essentially the same as those of Sec. 10.9, and the meanings of the symbols are given there. The four conditions above must be satisfied by the choice of five variables (three powers plus two spacings). There is one more variable than necessary; this “extra” is utilized in a later step to control one of the remaining aberrations (usually distortion). There are almost as many ways of solving this set of equations as there are designers. Stephens* has worked out the algebraic solution for the triplet, and his paper gives explicit equations for the values of the powers and spaces. An iterative approximation technique (which may be easily modified to apply to systems with more than three components) along the following lines is an alternate method, and its description will help to understand the limits and interrelationships involved in this design. 1. Assume a value for the ratio of the powers of elements c and a. This will be the “extra” degree of freedom mentioned above. (K  c/a  1.2 is a typical value.) 2. Choose a value (arbitrary) for a. (In the absence of prior experience, a  1.5 is suitable.) This determines c, since from step 1, c  Ka and also determines b, since Eq. 12.14 can be solved for b when a, c, h, and ∑PC are known or assumed. 3. Choose a value for S1 (one-fifth to one-tenth of the focal length is suitable). 4. Solve for the value of S2 which will satisfy Eq. 12.12 (assume that u′k is equal to ya). This is done by tracing a ray through elements a and b to determine ya, yb, and u′b. Then find S2 to yield the value of yc, which satisfies Eq. 12.12. (Note that S2 may have a negative value on the first try.)

*R. E. Stphens, J. Opt. Soc. Am., vol. 38, 1948, p. 1032.

The Design of Optical Systems: General

421

5. Trace a principal ray (thin-lens paraxial) through the desired stop position, which may be conveniently placed at element b to minimize the labor. Again assume u′k as in 4 and determine ∑TchC*. 6. Repeat from step 3 with a new choice for S1 until ∑TchC* is as desired. (As a second guess for S1, try the average of S1 and S2 from the first try.) 7. Determine the system power . If not as desired, scale the value of a used in step 2 and repeat from step 2 until a solution is obtained. Graphs of the relationships between S1 and ∑TchC* and between a and  are useful in steps 6 and 7. Element shape solution. When the element powers and spacings have been determined, there are three uncommitted degrees of freedom, namely the shapes of the three elements (plus the “extra,” K, mentioned in step 1 above). These variables must be adjusted so that the spherical, coma, astigmatism, and distortion are corrected to their desired values. Referring to the thin-lens contribution equations of Sec. 10.9, the aberrations can be seen to be quadratic functions of the element shapes; thus, a simultaneous algebraic solution cannot be used and some sort of successive approximation procedure is necessary. Thin-lens paraxial marginal and principal rays are traced through the three elements. The principal ray is traced so that the aperture stop is at lens b; both yp and Q for lens b will be zero.

1. Assume an (arbitrary) value for C1 and calculate TAC*a (the astigmatism contribution) for element a by Eq. 10.8h (a value of C1  2.5 is a reasonable first choice). 2. Since the stop is located at element b, TACb will not change with bending (Eq. 10.8o). Now solve Eq. 10.8h for the shape of element c, that is, the value of C5, which will give TAC*c which will yield the desired ∑TAC when combined with AC*a and ACb. Normally there are two solutions for C5 and the more reasonable one is used. 3. Now CC*a and CC*c (the coma contributions) are calculated from Eq. 10.8g. Since the equation for CCb is linear in C3 (Eq. 10.8n, since Qb  0), it can be solved for the unique value of C3 which will yield the desired ∑CC*. 4. The value of ∑TSC (spherical aberration) is now determined from Eq. 10.8m. 5. The procedure is repeated from step 1 with a new value of C1, and a graph of ∑TSC is plotted against C1. The shape C1 for which ∑TSC is equal to the desired value is chosen and the corresponding values

422

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of C3 and C5 are determined so that ∑TSC, ∑TAC*, and ∑CC* are simultaneously as desired. 6. If ∑DC* (distortion) is within acceptable limits, well and good; if not, a new power and space solution must be made with a different value of K  c/a. The value of ∑DC* can be plotted for several values of K as an aid in effecting a solution. Note that in step 5, there may be two, one, or no solutions for the desired ∑TSC. The best triplets seem to result from cases where the parabolic plot of ∑TSC just barely reaches the desired level. Step 6 also may have no, one, or two solutions. Thus, with two possible solutions in each of steps 2, 5, and 6, there are, theoretically at least, eight possible solutions for the thin-lens Cooke triplet. As indicated above, it is also possible that for a given set of conditions, there may be no solution. Usually, however, there is only one “reasonable” solution; occasionally there are two. The next step is the addition of thickness to the design. Center thicknesses for the crown elements are chosen to give workable edge thicknesses; the second surface curvatures (C2, C4, and C6) are adjusted to hold the thick-element powers exactly to the thin-lens powers. Airspaces are chosen so that the principal points of the elements are spaced apart by the thin-lens spacings. In this way, the thick-lens triplet will have exactly the same focal length as the thin-lens version. The thick lens is now submitted to a trigonometric raytrace analysis and the values of the seven primary aberrations are determined. If (as is likely) the aberrations are not as desired, a new round of design is initiated, with the new “desired” thin-lens aberration values adjusted to offset the difference between the raytracing results and the desired final values. For example, if the original “desired” ∑TSC was 0.2 and the raytracing yielded a marginal spherical, TAm  0.2, the new “desired” ∑TSC would be set at 0.4, assuming that the desired end result was TAm  0.0 In general, the initial choice for the “desired” third-order aberration sums should be small, undercorrected amounts, since the higher-order aberrations are usually overcorrecting. Spherical, Petzval, and axial chromatic follow this rule. Since the Cooke triplet is relatively symmetrical, the residuals of distortion, coma, and lateral color are small, and initial “desired” values of zero are appropriate. The desired Petzval sum should be definitely negative. For high-speed lenses, the Petzval radius is frequently as short as two or three times the focal length; moderateaperture systems (f/3.5) usually have !  3f to 4f; slow systems may have !  5f or longer. One reason for this relationship is that Initial choice of desired aberration values.

The Design of Optical Systems: General

423

the flatter (less undercorrected) the Petzval surface is made, the higher the element powers; hence the higher the residual aberrations, especially zonal spherical. The value chosen for the desired ∑PC is also an important factor in determining whether or not there is a solution for step 5 in the curvature determination process. The “desired” astigmatism sum is best set slightly positive, between zero and about one-third the absolute value of the Petzval sum, so that the inward curvature of the Petzval surface is offset by the overcorrected astigmatism. Glass choice. The choice of the glass to be used in the triplet is one of

the most important design factors. From field (Petzval) curvature considerations, it is desirable that the positive elements have a high index of refraction and the negative element a low one to reduce ∑/N. As usual, the V-value of the positive elements should be high and that of the negative element low in order to effect chromatic correction. For the positive elements, one of the dense barium crowns is the usual choice, although the light barium crowns on one hand and the rare earth (lanthanum) glasses on the other are frequently used. Although triplet designs are possible with ordinary crown glass or even plastics, their performance is relatively poor. It turns out that the interrelated requirements of Eqs. 12.11 through 12.14 lead to long systems (i.e., S1 and S2 are large) when the difference between the V-values of the positive and negative elements is large. A lens with a large vertex length will, at any given diameter, vignette at a smaller angle than will a short lens. Further, it turns out that the longer the lens: (1) the smaller the spherical zonal and (2) the smaller the field coverage (i.e., the higher-order astigmatism and coma are greater and limit the angle over which a good image can be obtained when the lens is long). Thus, long systems are appropriate for high-speed, small-angle systems; short systems for small-aperture, wide-angle applications. As a very rough rule of thumb, the vertex length of a triplet is frequently equal to the diameter of the entrance pupil. The length of the triplet can be controlled by the choice of the glasses used. For example, if a shorter system is desired, the substitution of a flint with a higher V-value (or a crown with a lower V-value) will produce the necessary change. To get a longer system, use a higher V-value crown and/or a lower V-value flint. (However, note that a system which is too long will have no solution for the element shapes. The ray height on the negative element may be so low that its overcorrecting contribution to the spherical aberration is insufficient to offset the undercorrection of the positive elements simultaneously with the requirements for coma and astigmatism correction as well as chromatic and Petzval.)

424

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Interestingly enough, this relationship between vertex length and zonal spherical and field coverage is a general one and applies to most anastigmats.* Thus, if an anastigmat design has too much zonal spherical and more than enough angular coverage, one can simply choose new glasses to lengthen the system and strike the desired balance between field and aperture, or vice versa. There are, of course, limits to the effectiveness of this technique. In general, the higher the index of the crown (positive) elements and the lower the index of the flint, the better the design will be. In other words, with all else equal, a triplet with a more positive index difference (n crown  n flint) will have a smaller zonal spherical and/or a wider field coverage. See also Fig. 13.52 for the effect of index on aberrations. Figure 10.9 showed a triplet of relatively high aperture and modest field coverage. Figures 12.13 and 12.14 illustrate triplets of reduced vertex length and increasingly smaller aperture and wider fields of view. Needless to say, the Cooke triplet is best designed using an automatic computer lens design program of the type described in Sec. 12.9. However, the automatic design program can be better utilized and better results will be obtained if the designer has mastered the information in this section. Figures 14.9 and 14.10 also show Cooke triplet designs. Figure 14.39 shows a triplet with an aspheric field corrector, suitable for use in a point-and-shoot camera, and Fig. 14.41 shows an infrared (8–14 m) triplet. Figure 14.42 is another IR triplet-based lens of very high speed (f/0.55). 12.8 A Generalized (Nonautomatic, OldFashioned) Design Technique The preceding sections have outlined specific design approaches for three particular types of optical systems. This section will describe a generalized approach to optical design. Because of the varied nature of different types of optical systems, this description will be unnecessarily elaborate for many simple cases and must, because of limitations of space and knowledge, fall short of completeness for elaborate and specialized systems. The reader will recognize generalizations of most of the procedures set forth in the preceding sections. This section describes the design process as if it were to be executed “manually,” i.e., without the benefit of a modern “automatic” optical design software program. The aim of this section is not necessarily to prescribe the operations indicated but to outline the structure of the

*See W. Smith, J. Opt. Soc. Am., vol. 48, 1958, pp. 98–105.

The Design of Optical Systems: General

Figure 12.13 A Cooke triplet anastigmat of moderate

aperture and coverage. Compare with Figs. 10.9 and 12.14. English Patent 155,640-1919. Focal length is 100 units. This design is of the type made for use in slide projectors.

Figure 12.14 A Cooke triplet of small aperture and wide cov-

erage. Compare with Figs. 10.9 and 12.13. German Patent 287,089-1913. Focal length is 100 units.

425

426

Chapter Twelve

basic design approach, including some techniques which may in fact be a valuable supplement to understanding and executing the design process. General considerations. The first step in the design process is the orga-

nization of the requirements to be imposed on the optical system into terms of aperture, focal length, field coverage, resolution (or blur spot size), spectral bandwidth, transmission, mechanical or space limitations, and the like. In some systems, e.g., telescopes, the preliminary design may be profitably carried out member by member; if this is to be done, requirements for the individual members are established. The general configuration of the system is established next. Ordinarily the designer will conduct a survey of known designs (books, technical periodicals, the patent files, and the designer’s own experience are the primary sources) to determine whether the performance requirements are within the “state of the art.” If so, the designer will select a type of system which is just capable of meeting the requirements (i.e., the most “economical” choice) and will proceed to adjust its parameters to achieve the optimum balance of correction for the particular application at hand. If the performance requirements are beyond the capability of any known design, the designer will select a design form which is felt to be “most likely to succeed.” The designer will analyze it thoroughly to determine its shortcomings and then attempt to improve its characteristics. In many instances, there is no directly applicable prior art from which to begin further effort. In such circumstances, a thorough analysis of the first-order (gaussian) requirements is conducted and a system is invented, utilizing the basic design principles exemplified in known designs on a piecemeal basis to accomplish the necessary ends. In the following paragraphs, we assume that the general design type has been established, either by selection or invention. The next major step in the design process is the correction of the primary aberrations, or at least as many of them as are necessary and feasible. This procedure has been accurately described as the art of solving a number (say n) of second- (or higher-) order equations in m unknowns; one must ascertain initially that m (the number of effective variables) exceeds or equals n (the number of aberrations). Manual correction of the primary aberrations. The powers and spacings

of the elements which are to comprise the system can usually be determined on a highly rational basis. First, the elements must be so arranged as to provide the desired focal length, aperture, field, and so on for the system. Throughout this entire design stage, the value of a scale drawing cannot be overemphasized; such a drawing will prevent

The Design of Optical Systems: General

427

attempts to design impossible elements, such as those with negative edge thickness, or with hyperhemispheric concave surfaces. If the ray paths are roughed in (on a first-order basis), one is also less apt to require magnifications and apertures which lead to slope or incidence angles which exceed 90°. The usual method for correction of the aberrations is bending the elements, i.e., changing the shape of the elements while maintaining a constant power and position. However, certain aberrations are unaffected (or affected only slightly) by bending. These are axial (longitudinal) chromatic aberration, lateral color, Petzval curvature, and, to a certain extent, distortion. The chromatic aberrations and the Petzval curvature must be corrected in the power and space layout if they are ever to be corrected. The third-order contribution equations, especially the thin-lens versions, are most useful at this stage, and it is ordinarily a relatively straightforward procedure to adjust the system so that the ∑TAchC, ∑TchC*, and ∑PC are equal to values which have been selected as desirable (or at least acceptable). See Eqs. 12.11 through 12.14. It then remains to correct the spherical, coma, astigmatism, and distortion to their desired values. A number of alternate procedures are often available at this step. Unless the designer has prior experience with the type of system under construction, or unless the design effort is a minor modification of an existing design, it is probably best at this stage to make a graph of the aberration contributions from each element (or component) as a function of the element shape. Then, from a set of such graphs, a region (or regions) in which a solution is possible can be selected. These graphs can be plotted from data obtained by the use of the thin-lens contribution equations, the surface contribution equations, or in some cases by direct raytracing. The latter two methods are appropriate for electronic computer work; one element at a time is bent and the changes in the final aberrations are plotted. The thin-lens expressions have the advantage that the “n equations in m unknowns” are explicitly that and can be handled analytically. When a “region of solution” is selected (by whatever means), a method of differential correction is usually applied. The partial differentials of the aberrations against shape, A/C (or A/ C), are determined along with the values of the aberrations for a trial prescription. The desired amount of change of each aberration ( A) is determined from the analysis of a trial prescription and the necessary number (n) of simultaneous equations of the general form iK

An 

C 冱 冢 C 冣 i1 An

i

i

(12.15)

428

Chapter Twelve

are set up and solved to yield the required values of Ci. Because of the nonlinearity of the equations (i.e., the partials vary as the shape is changed), the first solution is seldom precise. However, the preselection of the region of solution limits the size of the C’s so that the linear simultaneous solution of Eqs. 12.15 is a good approximation; a series of such solutions converges rapidly on the required design form. It is sometimes advisable to limit the number of parameters used in the technique described above. Because a limited number of aberrations are to be controlled, the problem is simplified if only an equal number of variables are used, provided that these variables are effective and admit of a solution. The preliminary graphs of the aberrations (versus element shapes) and the subsequent selection of a region of solution are strongly recommended as insurance against ineffective parameters and insoluble sets of simultaneous equations. Certain systems lend themselves to an iterative technique which can be a powerful design tool. For example, assume that three aberrations, A, B, and C are to be corrected by the adjustment of three parameters, x, y, and z. An initial trial prescription is modified by changing one of the parameters, say z, until one of the aberrations, say C, is “corrected.” Then parameter y is arbitrarily changed and a new value of z is determined to maintain the correction of C. Parameter y is varied in this manner until the aberrations B and C are simultaneously corrected. Then parameter x is changed; with each change of x, parameters y and z are adjusted as above to hold the aberrations B and C at the desired values. Parameter x is varied in this manner until aberration A is brought to correction simultaneously with B and C. In such a process, graphs of C means z, B versus y, and A versus x are quite useful. If the thin-lens aberration expressions have been used in any of the preceding steps, it is necessary to add thickness to the elements. This is generally done by adjusting the secondary curvature of each thick element to hold the thick-element power equal to the thin-lenselement power. The spacing between elements is then adjusted so that the spacing of the thick-element principal points is equal to the thinlens spacing. This method serves to retain the overall system power and working distances at the same values as the thin-lens systems. Some designers prefer to adjust the secondary curvatures to maintain the Petzval curvature precisely. The exact procedure used to go from thin to thick is not critical; what may be important is that the procedure of introducing thickness be rigorously consistent (in order that the differential trigonometric correction method will be accurate). Trigonometric correction. When the third-order aberrations have been

brought to desired values, it is necessary to trace rays trigonometrically to determine the actual state of correction of the system. It will

The Design of Optical Systems: General

429

usually differ by a small amount from that predicted by the third-order aberrations. However, a step or two of differential correction as outlined five paragraphs above will usually bring the trigonometric correction home; in most systems, the change in the trigonometrically determined aberrations is quite close to the change predicted by thirdorder aberration calculations. Reduction of residual aberrations. After the primary aberrations have

been brought to correction, the design is tested for residual aberrations. The primary aberrations are generally corrected for only a single zone of the aperture or field and can be expected to depart from correction in all other zones, as previously discussed in Chapter 3. Several general principles can be given for the reduction of residuals; their variety and extent make a catalog of specific remedies too extensive for inclusion. If there are any “leftover” parameters that were not used in the correction of the primary aberrations, these may be systematically varied and their effects on the residuals noted and used. In addition to the obvious and continuously variable parameters of bendings, powers, and spacings, the choice of glass types is often an effective leftover. Also the possibility that more than one region of solution exists should not be overlooked, since this is, in effect, an extra parameter. An analysis of the source of the third-order surface contributions will often pinpoint one or two surfaces or elements which are especially heavy contributors. The elimination or reduction of a single large contribution will often reduce residual aberrations. This can be accomplished by introducing a correcting element near the offender (for example, convert a single element into a compound component, perhaps an achromat), by splitting the offending element into two elements whose total power equals that of the original, by raising the index, or (infrequently) by shifting the offender to a location where the incidence angles of the rays on its surfaces are reduced. Compounding or splitting an element introduces two new variable parameters: the ratio of the powers of the two elements (although the best split ratio is often close to 50-50) and the shape of the added element. An additional possibility is that a drastically different shape for the troublesome element may reduce its contribution to an acceptable level. The specific remedies for spherochromatism, zonal spherical, and field coverage set forth in Secs. 12.5 and 12.7 have fairly general applicability. Another specific is the introduction of a zero-power meniscus element or a concentric meniscus element into the system. Depending on how and where it is used, a meniscus can be effective in modifying zonal spherical, Petzval curvature, or astigmatism.

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An aspheric surface can be a powerful design tool for the reduction of residuals or the elimination of primary aberrations (especially distortion, astigmatism, and spherical) which will yield to no other design techniques. One should, if at all possible, temper one’s enthusiasm for the easy way out which the aspheric surface represents with the knowledge that several spherical elements may usually be added to a design for less than the cost of producing a single precise aspheric surface. As a consequence of this fact, aspherics are seldom used except where absolutely necessary for space or weight considerations, or where cost is no object (as in one-of-a-kind instruments), or where the required precision of the surface is very low (as in molded condenser elements). Although injection-molded plastic element and diamondturned surfaces are often aspheric, and glass aspherics can be molded, tooling cost is the limitation here. In general, where residuals are a problem, it is wise to reconsider the initial power and space layout for the entire system. It is sometimes possible to revise the layout in such a way that the powers of the elements or the “work” (y or yp) done by the elements can be reduced. This is an extremely rapid and effective way of reducing residuals. An initial choice of too small a value for the Petzval sum will result in elements of high power and large residuals. A change to allow a more inward-curving field is the obvious remedy for this situation for ordinary lenses. Aberration balancing. The final stage in the optical design process con-

sists of balancing the aberrations, or “touching up” the design. Here the experienced designer frequently departs from what may seem to be the best state of correction in order to minimize the overall effects of the residual aberrations. In the presence of zonal spherical, spherochromatism, and astigmatism, the interrelationships of the aberrations with each other, and with the position selected for the focal plane, often allow an improvement to be made by selecting a deliberately uncorrected state. We have previously (Sec. 11.3) seen that the best spherical correction as regards OPD occurs when the marginal spherical is zero and the reference plane is shifted toward the zonal focus; the minimum geometrical blur spot size (Sec. 11.7) requires that the marginal spherical be undercorrected. Thus, if the application of the system is such that a resolution significantly less than the diffraction-limited resolution is of prime importance, and if the zonal spherical is large in terms of OPD, then an undercorrected marginal spherical is in order. Except in a camera lens, an overcorrected marginal spherical is rarely desirable; it does permit a higher resolution and reduces focus shift when the system is stopped down, but it reduces the image contrast.

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Another reason for preferring a slightly undercorrected spherical is that the oblique spherical aberration (y3h2) is almost always overcorrected and the axial undercorrection will counterbalance this tendency. The overcorrected oblique spherical also causes the effective field curvature to be more backward-curving than indicated by the xs and xt curves given by Coddington’s equations (Eq. 10.5). This is especially true for the tangential field curvature. For this reason the astigmatism is seldom made overcorrected enough to cause a backwardcurving tangential field; ordinarily one desires a correction somewhere between xt  0 and xt  xs  xp. Note that the focus position is usually chosen inside the paraxial focal plane and that the field curvature should be judged with this in mind. We have previously noted that the Petzval curvature in most anastigmats is preferably left somewhat inward-curving in order to minimize element powers and aberration contributions. The obvious choice of the 0.707 zone of the aperture as the zone at which to correct the longitudinal chromatic is rarely the best choice unless the spherochromatism is small. In the presence of spherochromatism and an undercorrected zonal spherical, the inward shift of the best focus from the paraxial focus allows the overcorrected spherical of the blue light to produce a halo or blue haze in the image. This can be eliminated, or reduced, by correcting the chromatic at a larger zone of the aperture. The reader should bear in mind that the preceding comments are intended to apply to normal types of lenses in which (as is usually the case) the higher-order residuals are somewhat larger than desirable. 12.9 Automatic Design by Electronic Computer The fantastically high computation speed of the electronic computer makes it possible to perform a major portion of the optical design task on an “automatic” basis. One possible approach is essentially a duplication of the process that a designer goes through in correcting the primary aberrations of a system. The computer is presented with an initial prescription and a set of desired values for a limited set of aberrations. The machine then computes the partial differentials of the aberrations with respect to each parameter (curvature, spacing, etc.) which is to be adjusted and establishes a set of simultaneous equations (Eqs. 12.15), which it then solves for the necessary changes in the parameters. Since this solution is an approximate one, the computer then applies these changes to the prescription (assuming that the solution is an improvement) and continues to repeat the process until the aberrations are at the desired values. When there are more variable

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parameters than system characteristics to be controlled, there is no unique solution to the simultaneous equations; in this case, the computer will add another requirement, namely that the sum of the squares of the (suitably weighted) parameter changes be a minimum. This allows a solution to be found and has the added advantage that it holds the system close to the original prescription. Since the solution of simultaneous equations may call for excessively large changes to be applied, the computer is usually instructed to scale down the changes if they exceed a certain predetermined value. This “simultaneous” technique is a useful one. Even modest-sized computers are capable of handling this problem without difficulty and several inexpensive computer programs of this type are available, often based on third-order aberration contributions. Since the designer is in rather close control of the situation, this technique is, in effect, simply an automation of conventional methods as described in the preceding section. Thus, the designer should have a fairly good knowledge of the system, and the system must have a solution reasonably close to the initial prescription. This type of approach is very efficient for making modest changes in designs or for touching-up a design. It also makes easy work of systems with exceedingly complex interrelationships of the variables, such as the older meniscus anastigmats of the Dagor or Protar type. Fully automatic lens design optimization

There are many other approaches to automatic design; almost all of them are characterized by the use of a “merit function.” The merit function is a single numerical value which indicates to the computer whether any given change has improved the lens or not. Obviously, representing the total performance of a lens system by a single number is a rather tricky business and considerable care must be taken in the choice of the merit function; at times it seems that the “design” of the merit function is more demanding than the design of the lens which the merit function is intended to represent. Some approaches use a merit function of the following sort: A large number of rays are traced from each of several points in the field of view. For each image point, the distance of each ray intersection (with the image plane) from the “ideal” location for that ray is computed and the sum of the squares of these distances is taken. Then the sum of the sums for the several image points is the merit function. Since the merit function will be large if the image blur spot is large, it is apparent that a small value of the merit function is desirable. The construction of the merit function as described above is far from the most desirable scheme of things, and in practice many refinements are used. Since the outer portions of the field are frequently less criti-

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cal than the center, the individual sums may be weighted to take this into account. A modest amount of computation will indicate that, in the presence of a constant fifth-order spherical aberration, the smallest value of the sum of the squares of the ray displacements does not represent the best solution from an OPD standpoint. One scheme uses a reduced weighting of large ray displacements in an attempt to take this into account. The choice of the “ideal” intersection point for the rays (for off-axis points) is a complex matter; the use of the gaussian image point is quite misleading if any amount of distortion is present. Similarly, the use of the image-plane intersection of the principal ray as the ideal point can yield a distorted evaluation in the presence of coma. Frequently the separately computed values of distortion and lateral chromatic aberration are added (suitably weighted) into the merit function, and the computer selects the centroid of the blur spot as the “ideal” point. Other types of merit function are also widely used to characterize the quality of a lens system. A few use the OPD, or wave-front aberration, as the merit function, taking the variance of the wave front for several field points, after selecting the reference point (i.e., image plane) so as to minimize the variance over the field. Another very widely used approach allows the designer to tailor a merit function to suit the application. The merit function entries may be ray displacements, OPD, defocusing, field curvature, chromatic aberrations, the slope, or the curvature of the ray intercept plot, the constructional data of the lens, the ray heights or slopes, or the classical aberrations, plus almost any mathematically possible combination of these. The merit function, being a collection of aberrations and departures from desired conditions, is obviously misnamed; it properly should be called a defect function or error function. However, common usage has established “merit function” as a well-understood term, and we will use it here with the understanding that the smaller the merit function, the better the image. Almost all automatic-lens-design programs allow at least some adjustment to the merit function, even if they do not allow the sort of flexibility described above. Typically, even in a program of limited flexibility, different parts of the aperture, field, or spectrum can be weighted to suit the application and the design form. The general procedure is to have the program optimize a design, for the designer to examine the results, and then to adjust or alter the merit function in such a way as to achieve the desired balance of aberrations and characteristics. Automatic-lens-design programs operate this way: Each of the construction parameters to be varied is changed (one at a time) by a small amount. The corresponding change in each entry or aberration in the merit function is calculated in order to obtain its partial derivative

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with respect to the parameter. Then equations of the form of Eqs. 12.15 are set up, one for each aberration or merit function entry. Typically there are many more aberrations in the merit function than there are effective variable parameters in the lens, so a “solution” is made in the least-squares sense, i.e., the variable set is changed in such a way as to minimize the sum of the squares of the differences between the desired value of each aberration and the value predicted by Eqs. 12.15. But Eqs. 12.15 are based on an approximation; the assumption that the relationship between aberration and variable is a linear one. We have seen in Chapters 3 and 10 that, even for thirdorder aberrations, this is not so, and it is much less linear for the higher-order aberrations. At best then, the solution is an approximate one, but probably significantly improved over the original lens form. At worst, the nonlinearity of the relationships can cause the least-squares process to come up with such an extreme change that the design is not just worse, it may be a totally impossible form with near-zero radii that the rays miss, or near-infinite spacings that cause similarly disastrous results. This problem can be handled by adding to the merit function the sum of the weighted squares of all the parameter changes. This penalizes any large parameter changes and tends to stabilize the process. The weighting can be adjusted to be large where the nonlinearity is a problem, and small where it is not. This is called damped least squares, and with a few significant exceptions, is the basis of current automatic lens design programs. By repeating the approximate solution process until it converges, these programs are capable of driving a rough preliminary design form to the nearest local minimum of the merit function. Depending upon the structure of the merit function, most lens designs have more than one local minimum. Consider the “front” and “rear” meniscus camera lens discussed in Sec. 12.2, or the Fraunhofer and Gauss forms of telescope objectives (Secs. 12.4 and 12.5); these are simple design forms where the merit function has two obvious local minima. An automatic design program will find the minimum nearest to the starting design form which it is given. There is no way that the user of such a program can be certain that a minimum is the best one (i.e., a “global optimum”). The solution space is n-dimensional, where n is the number of variable parameters. In the simple designs discussed in this chapter it was not impractical for us to do a limited, simplified exploration of the solution space. In a design with 20 or 30 variable parameters it is a quite different matter. In any case, it is apparent that since the design program will seek out the nearest minimum, the selection of the starting point for the process is vitally important. In fact, once the merit function is defined and weighted, the starting design form uniquely defines a single min-

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imum. Obviously the choice of the starting form is a critical factor. Fortunately, it seems that with most merit functions, most nonsimple design types have relatively broad, flat minima, and one can choose a starting point over a fairly large volume in solution space and expect a reasonably good result. An experienced lens designer uses knowledge of successful design types and features to direct the computer to good starting points. The novice designer should study the standard, classical design forms as an aid in selecting appropriate starting points. The mathematics of this process are written up in many places. Two which explain the basic operations are G. Spencer, “A Flexible Automatic Lens Correction Procedure,” Applied Optics, vol. 2, 1963, pp. 1257–1264, and W. Smith, in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. 12.10

Practical Considerations

The following is a partial list of certain design characteristics which, although they may be quite beneficial to the performance of a design, tend to have an undesirable effect on the difficulty and cost of fabrication. Thus, unless you enjoy being unpopular with the opticians who must execute your designs, this list represents things which you should assiduously avoid if at all possible. 1. Materials which are soft and easily abraded. 2. Materials which are thermally fragile and which may split from a mild thermal shock, such as that encountered in blocking or washing under a hot or cold water tap. 3. Materials with low acid resistance or high stain characteristics. 4. Expensive materials. (Often you can find a similar, cheaper glass which is nearly as good.) 5. Thin elements, i.e., those with a large ratio of diameter to the average thickness. Such elements can deform under the stress of blocking or polishing, making an accurate surface geometry almost impossible to produce. Note that a negative element with a substantial edge thickness often can tolerate a center thickness which would be too thin for a weaker element. 6. Thin-edged elements chip easily and, if processed at a diameter larger than the finished one, may become sharp-edged during fabrication. Also a thin-edged element is difficult to mount satisfactorily. 7. A very thick element obviously requires more material and may require an awkward arrangement when blocked. Visualize Fig.

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15.2 if the elements are as thick as the diameter. A thin lens with the same radius can have more lenses blocked on a tool because they can be placed closer together at the surface; with the thick lens, there are large gaps between the elements at the surface which make polishing difficult. 8. Very “strong” curves (i.e., with a large diameter-to-radius ratio) lead to fewer elements blocked per tool and the correspondingly increased processing costs, difficulty in polishing surfaces accurately, and difficulty in testing the surface accuracy with a test plate or interferometer. 9. Meniscus elements whose surfaces are concentric or nearly concentric with each other. A monocentric element must be ground and polished so that the two surfaces are properly aligned during these operations; it cannot be “centered” after polishing as an ordinary element can. 10. Nearly equiconvex or equiconcave elements can cause trouble in assembly because it is difficult to tell one side from the other, and the element is liable to be mounted backward. 11. Weakly curved, nearly plane surfaces are more expensive to tool and fabricate than a plane surface. It is almost always possible to force such a design to a plane surface with little or no sacrifice in image quality. 12. Precision bevels. If possible, avoid mounting from a beveled surface. Use a loosely toleranced 0.5 mm by 45° chamfer to eliminate sharp edges; this kind of edge break is almost free. 13. Avoid odd-angle precision bevels. Many shops are tooled for 45°, 30°, or 60°; other angles may require new tooling. 14. Cemented triplets and quadruplets are unpopular in some shops. 15. Tight scratch and dig specifications on surfaces which are not visible to the ultimate customer are usually a waste of money. With a few exceptions (such as surfaces near an image plane or the optics of a high-powered laser system), scratch and dig considerations are purely cosmetic and have no functional effect (unless the lens aperture is so small that a dig can actually obstruct a significant fraction of the beam area). 16. Tight tolerances in general. See Chap. 15 for a discussion of efficient tolerance budgeting. Bibliography Note: Titles preceded by an asterisk (*) are out of print.

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*Conrady, A., Applied Optics and Optical Design, Oxford, 1929. (This and vol. 2 were also published by Dover, New York.) *Cox, A., A System of Optical Design, Focal, 1965 (lens construction data). Dictionary of Applied Physics, vol. 4, London, Macmillan, 1923. Farn, M. W., and W. B. Veldkamp, “Binary Optics,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 8. Fischer, R. (ed.), Proc. International Lens Design Conf., S.P.I.E., vol. 237, 1980. *Greenleaf, A., Photographic Optics, New York, Macmillan, 1950. Herzberger, M., Modern Geometrical Optics, New York, Interscience, 1958. *Jacobs, D., Fundamentals of Optical Engineering, New York, McGraw-Hill, 1943. *Kingslake, R. (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965 (lens design). *Kingslake, R., Lens Design Fundamentals, New York, Academic, 1978. *Kingslake, R., Lenses in Photography, Garden City, 1952. *Linfoot, E., Recent Advances in Optics, London, Clarendon, 1955. *Martin, L., Technical Optics, New York, Pitman, 1950. Merte, W., Das Photographische Objektiv, Parts 1 and 2, translation, CADO, Wright-Patterson AFB, Dayton, 1949. Merte, Richter, and von Rohr. Handbuch der Wissenschaftlichen und Angewandten Photographie, vol. 1, 1932; Erganzungswerke, 1943, Vienna, Springer. Reprinted by Edwards Brothers, 1944 and 1946 (lens construction data). Merte, The Zeiss Index of Photographic Lenses, vols. 1 and 2, CADO, Wright-Patterson AFB, Dayton, 1950 (lens construction data). MIL-HDBK-141, Handbook of Optical Design, 1962. Peck, W., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (automatic lens design). Rodgers, P., and M. Roberts, “Thermal Compensation Techniques,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 39. Rosin, S., “A New Thin Lens Form,” J. Opt. Soc. Am., vol. 42, 1952, pp. 451–455. Sinclair, D. C., “Optical Design Software,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 34. Smith, W. J. (ed.), Lens Design, S.P.I.E., vol. CR41, 1992. Smith, W. J., Modern Lens Design, New York, McGraw-Hill, 1992. Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985.

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Taylor, W., and D. Moore (eds.), Proc. International Lens Design Conf., S.P.I.E., vol. 554, 1985. Exercises The exercises for this chapter take the form of suggestions for individual design projects; as such, there can be no “right” answers, and none are given. The effort involved in each exercise is considerable, and it is likely that only those interested in obtaining first-hand experience in optical design will wish to undertake these exercises. The casual reader will, however, be amply rewarded by mentally reviewing the steps he or she would follow in attempting the exercises. 1 Design a symmetrical double-meniscus objective of the periscopic type. Select a bending (a ratio of 3:2 for the curvatures is appropriate), determine the proper spacing for a flattened field, and calculate the thin-lens third-order aberrations for the combination. Analyze the final design by raytracing and compare the results with the third-order calculations. The student may wish to repeat the process for several additional bendings, perhaps including the Hypergon (Fig. 12.4), and to compare the results of each, noting the variations of aperture and coverage. 2 Design an achromatic doublet objective using BK7 (517:642) and SF2 (648:339). Correct the spherical aberration for an aperture of f/3.5. Raytrace marginal and zonal rays in C, D, and F light to evaluate the axial image. Compare the coma obtained by raytracing an oblique fan with the OSC calculation. 3 Design a telescope objective lens consisting of a BK7 singlet and a doublet of BK7 and SF2. Vary the distribution of powers and the spacing to optimize the correction of zonal spherical and spherochromatic. 4 Design a Cooke triplet anastigmat. For a minimal exercise, duplicate the design of Fig. 12.13 using the same glasses and the same power and space layout as a starting point. For a more ambitious project, design the same lens, but derive the power and space layout without recourse to the data of the figure.

Chapter

13 The Design of Optical Systems: Particular

13.1

Telescope Systems and Eyepieces

The design of a telescopic system begins with a first-order layout of the powers and spacings of the objective, erectors, field lenses, prisms, and eyepiece, as required to produce the desired magnification, field of view, aperture (pupil), eye relief, and image orientation. Then the individual components are designed so that the telescope, as an entire system, is corrected. Usually the eyepiece is designed first; the design is carried out as if the eyepiece were imaging an infinitely distant object through an aperture stop located at the system exit pupil. That is, the rays are traced in the reverse direction from the direction in which the light travels in the actual instrument. Usually a principal ray is traced from the objective (or the aperture stop) through the eyepiece to locate the exit pupil, then an oblique bundle can be traced in the reversed direction (from the eye) to evaluate the off-axis imagery. Almost all optical design is done in this manner, by tracing rays from long conjugate to short, largely for convenience, because the focus variations (due to aberrations and small power changes) are smaller and more readily managed at the short conjugate. The erectors, if there are any, are usually designed next; their design is frequently included in the eyepiece design by considering the erector and eyepiece as a single unit. (Alternatively, the erector may be considered as a part of the objective; the choice is usually determined by the location of the reticle.) Usually the objective is designed last and 439

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its spherical and chromatic aberrations are adjusted to compensate for any undercorrection of the eyepiece. Note that prisms must be included in the design process if they are “inside” the system, since they contribute aberrations which must be offset by the objective and eyepiece. Prisms can be introduced into the calculation as plane parallel plates of appropriate thickness. An eyepiece is a rather unusual system, in that it must cover a fairly wide field of view through a relatively small aperture (the exit pupil) which is outside the system. The external aperture stop and wide field force the designer to use care with regard to coma, distortion, lateral color, astigmatism, and curvature of field; the first three mentioned can become unusually difficult, since even approximate symmetry about the stop (which is used in many lens systems to reduce these aberrations) is not possible. On the other hand, the small relative aperture of an eyepiece tends to hold spherical and axial chromatic aberrations to reasonable values. Typically an eyepiece is fairly well corrected for coma for one zone of the field (a fifth-order coma of the y2h3 type is common in wide-angle eyepieces) and the field is sometimes artificially flattened by overcorrected astigmatism which offsets the undercorrected Petzval curvature. Lateral color may or may not be well corrected; frequently some undercorrection exists to offset the effect of prisms. There is almost always some pincushion distortion apparent (note that when an eyepiece is traced from long to short conjugate, the sign of the distortion is reversed). An eyepiece can be considered “reasonably” corrected for distortion if it has 3 to 5 percent; 8 to 12 percent distortion is not uncommon in eyepieces covering total fields of 60° or 70°. One way to eliminate this distortion is by the use of aspheric surfaces, a not very attractive solution unless molded plastic or glass is used. One should remember that, in many applications, the function of the outer portion of the field of view is to orient the user and to locate objects which are then brought to the center of the field for more detailed examination. Thus, eyepiece correction off axis need not be as good as that of a camera lens, for example. Because the eyepiece is subject to a final evaluation by a visual process, it is sometimes difficult to predict, from raytracing results alone just what the visual impression will be. For this reason, it is frequently useful to begin an eyepiece design on the lens bench, by mocking up an eyepiece out of available elements. A series of mockups will yield a good grasp of the more promising orientations and arrangements of the elements. The designer can then use these as starting points for the design effort with reasonable assurance that the visual “feel” of the finished design will be acceptable. Note that the conventional correction of distortion (where h  f tan $) causes the apparent angular size of the image to change as it is

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scanned across the field. A distortion which yields the relationship h  f $ will give a constant angular size; this is a common type of distortion for many eyepieces. Field curvature causes a “swimming” effect of the image as the eye is scanned across the system pupil. Usually a field curvature of about 2 diopters or less (at the eye) is considered good; 4 diopters is about the maximum acceptable. The Huygenian eyepiece. The Huygenian eyepiece (Fig. 13.1a) consists

of two plano-convex elements, an eyelens and a field lens, with the plane surface of each toward the eye. The focal plane is between the elements. For a given set of powers of the elements, the spacing can be adjusted to eliminate lateral color. The required spacing is approximately equal to the average of the focal lengths of the elements. The only remaining degree of freedom is the ratio of powers between the elements. This is used to eliminate coma (and thus artificially flatten the field via the “natural” stop position, as discussed in Sec. 12.2). Since the image plane is between the lenses and is viewed by the eyelens alone, it is not well corrected and is unsuitable for use with a reticle. The eye relief of the Huygenian is often uncomfortably short. The Ramsden eyepiece. The Ramsden eyepiece (Fig. 13.1b) also con-

sists of two plano-convex elements, but the plane surface of the field lens faces away from the eye. The spacing is made about 30 percent shorter than the Huygenian to allow an external focal plane, and for

Figure 13.1 Three basic eyepiece

forms.

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this reason lateral color is not fully corrected. Coma is corrected as in the Huygenian by varying the ratio of field lens power to eyelens power. The Ramsden eyepiece can be used with a reticle. The Kellner eyepiece. The Kellner (Fig. 13.1c) is simply a Ramsden

eyepiece with an achromatized eyelens to reduce the lateral color. It is frequently used in low-cost binoculars. The relative characteristics of the three simple eyepieces described above are summarized in the table of Fig. 13.2. They are almost invariably made in plano-convex form and little is gained by departing from this form. Since these eyepieces are chiefly noted for their low cost, the usual material for the single elements is common crown; indeed, they are frequently made from selected window glass by grinding and polishing only the convex surface. In the Kellner eyelens, the index difference across the cemented face is critical; usually a light barium crown is used to keep the overcorrection of the astigmatism from becoming too large when a wide field of view is desired. Departure from the plano-convex form, in favor of a biconvex shape, is not uncommon in the Kellner eyepiece. The half-field covered by these eyepieces is to the order of ±15°, more or less, depending on the performance required. The orthoscopic eyepiece. The orthoscopic eyepiece (Fig. 13.3a) con-

sists of a single-element eyelens (usually plano-convex) and a cemented triplet (usually symmetrical). The eyelens is frequently of light

Figure 13.2 The relative characteristics of three simple eyepieces.

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Figure 13.3 Eyepiece designs. (a) Orthoscopic; (b) symmet-

rical; (c) Erfle; (d) Erfle; (e) Berthele; (f) see also Fig. 14.6 for an example of this design.

barium crown or light flint glass and the triplet is composed of borosilicate crown and dense flint glass. This is a better eyepiece than the preceding simple types and is used for half-fields of ±20° to ±25°. The Petzval curvature is about 20 percent less than that of the Ramsden or Kellner, although higher-order astigmatism causes a strongly backward-curving tangential field at angles of more than 18° or 20° from the axis. (This high-order astigmatism is the characteristic which limits the field coverage of most eyepieces; some control can often be achieved by lowering the index difference across cemented surfaces.) The eye relief is long, to the order of 80 percent of focal length. Distortion correction is quite good. The symmetrical, or Plössl, eyepiece. This excellent eyepiece is com-

posed of two achromatic doublets (usually identical) with their crown elements facing each other (Fig. 13.3b). It is usually executed in borosilicate crown (517:642) and extra dense flint (649:338) glass, although it can be improved a bit by raising the index of both elements. It shares the long eye relief (0.8F) and field characteristics of the orthoscopic, but is in general a somewhat superior eyepiece, except that its distortion is typically 30 to 50 percent greater than the orthoscopic. It is widely used in military instruments and as a generalpurpose eyepiece of moderate (to ±25°) field. A similar eyepiece with

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both flints facing the eye is occasionally used. See Fig. 14.7 for an example of a symmetrical eyepiece. The Erfle eyepiece. This eyepiece (Fig. 13.3c) is probably the most

widely used wide-field (±30°) eyepiece. The eye relief is long (0.8F), but working distance is quite short. The Petzval sum is about 40 percent less than the orthoscopic or symmetrical types because of the fieldflattening effect of the concave field lens surface, and distortion is about the same as the orthoscopic (for the same angular field). The type shown in Fig. 13.3c usually has undercorrected lateral color (for use with erecting prisms) which can be reduced by use of an achromatic center lens as in Fig. 13.3d. Glasses used are usually dense barium crown and extra dense flint. An example of an Erfle eyepiece is shown in Fig. 14.8. Magnifiers and viewer lenses are basically the same as eyepieces, with one notable exception: There is no fixed exit pupil. This means that the eye is free to take almost any position in space and therefore the aberrations of the magnifier must be insensitive to pupil shift. For this reason, magnifiers tend to be symmetrical in configuration. Two plano-convex lenses with convex surfaces facing or a symmetrical (Plössl) construction are common for better-grade magnifiers. Where cost is important and a single element must be used, the following arrangements are good. If the eye is always close to the magnifier, use a plano-convex form with the plano surface toward the eye. If the eye is always far from the magnifier, use a plano-convex form with the convex surface toward the eye. If the eye position is variable, as in a general-purpose magnifier, an equiconvex form is probably the best compromise. Figure 14.5 is an example of a doublet magnifier. Note that the eyepieces of instruments which use an electronic image tube, such as the Sniperscope, fall into the category of magnifiers, since they are used to view a diffuse image on the phosphor surface of the image tube. As such they must be designed so that they perform well with the eye in a wide range of locations. The optics of tabletop slide viewers, “head-up displays,” or HUDs, and many simulators not only fall into this category but also share the requirement that both eyes view the image through a single optical system. Such systems are called biocular (as opposed to binocular systems, in which both eyes are used, but in which each eye views the image through a separate optical train). In a biocular system one must not only be concerned about the effects of eye motion but must also be concerned about any disparity between the images as seen by the two eyes. The convergence, divergence, and dipvergence (the vertical difference in direction) required of the eyes as they view the image must Magnifiers.

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be carefully considered in designing the system. Thus a biocular device is designed for a pupil large enough to encompass both eyes plus any head motion, although the image sharpness and resolution are determined by the aberrations of a pupil whose size is defined by that of the viewer’s eye. In binocular systems, one eyepiece is usually focusable to compensate for any difference in focus between the two eyes. The motion of the eyepiece is Diopter adjustment (focusing) of eyepieces.

  0.001f 2D millimeters or   0.0254f 2D inches where f is the eyepiece focal length, and D is the shift of the image position in diopters (relative to the second focal point of the eyepiece— where the eye is presumed to be located). The usual adjustment range is ±4 diopters. Erectors. Erector systems come in all sizes and shapes. Occasionally

a single element may serve as an erector, or two simple elements in the general form of a Huygenian eyepiece may be used, as in the terrestrial eyepiece shown in Fig. 13.4a. This form of eyepiece is widely used in surveying instruments, occasionally with an achromatic eyelens. A popular erector for gun scopes is illustrated in Fig. 13.4b and consists of a single element plus a low-power, overcorrecting doublet, often meniscus in shape. Photographic objective systems are occasionally used as erectors, symmetrical forms of the Cooke triplet, the Dogmar, or the double-Gauss being the most popular. Probably the most widely used erector consists of two achromats, crown elements facing, with a modest spacing between them. As previously mentioned, erectors are usually designed in conjunction with either the eyepiece or objective of a telescopic system. Considerable care should be taken in the first-order layout of any telescope to be certain that the work load placed on the erector is not impossibly large. The introduction of suitable field lenses is often necessary to reduce the height of the principal ray at the erector, although this does produce an undesirable increase in the Petzval curvature. Note that many erectors have external pupils, often in the form of a glare stop. Objective systems. For most telescopic systems, the objective will be an ordinary achromatic doublet, or one of the variations described in

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Figure 13.4 Erector systems. (a) The four-element terrestri-

al erecting eyepiece. (b) Typical gunsight optical system. (c) Symmetrical doublet erector.

Sec. 12.5. A photographic-type objective may be used where a wide field is desired, Cooke triplets and Tessars being the most commonly used. A Petzval objective is useful when high relative apertures are necessary; the construction of a Petzval objective (Sec. 13.3) is such that its rear lens acts as a sort of field lens, and this characteristic is occasionally useful. For high-power telescopes where it is desirable to keep the system as short as possible, a telephoto type of construction is valuable. The front component is an achromatic doublet and the rear is a negative lens, either simple or achromatic. The focal length is usually 20 to 50 percent longer than the overall length of the objective. Either the Petzval or telephoto type of objective can be used as an internal focusing objective (Fig. 13.5), where focusing is accomplished by shifting the rear (inside) component, making a more easily sealed instrument. Surveying instruments and theodolites conventionally use the telephoto form with the focusing lens located about two-thirds of the way from the front component to the focal plane so that the stadia “constant” will remain constant as the instrument is focused. Alignment telescopes use a positive focusing lens of high power placed near the focal plane at infinity focus; thus, a modest shift of the focusing lens toward the front component allows the system to be focused at extremely short distances, or even on the objective itself. Note that any system which works over a wide range of magnifications (as this type

The Design of Optical Systems: Particular

447

Figure 13.5 Telescopic systems. (a) Typical surveying telescope with

negative focusing lens and terrestrial eyepiece. Note that the objective is telephoto, in that its effective focal length is longer than the objective. (b) Alignment telescope. The strong positive focusing lens, when shifted forward, allows the instrument to focus at extremely short distances.

of focusing lens does) should be designed so that the change of aberration contribution is small as the magnification is varied. 13.2

Microscope Objectives

Microscope objectives (Fig. 13.6) may be divided into three major classes: those designed to work with the object under a cover glass, those designed to work with no cover glass, and immersion objectives, which are designed to contact a liquid in which the object is immersed. All types are designed by raytracing from the long conjugate to the short; the effects of the cover glass (when used) must be taken into account by including it in the raytrace analysis. Standard cover glass thickness is 0.18 mm (0.16 to 0.19 mm, n  1.523 ± 0.005, v  56 ± 2). Microscope objectives are designed to work at specific conjugates, and their correction will suffer if they are used at other distances. For cover glass objectives and immersion objectives, the standard distance from object plane to image plane is 180 mm. For metallurgical types (no cover glass), the standard distance is 240 mm. The chief effect of changing the tube length or cover glass thickness from its nominal value is to overcorrect or undercorrect the spherical aberration; an objective which has been improperly adjusted at the factory may be reclaimed by using a nonstandard tube length or cover glass if the defect is not too serious. Note that ordinary microscope objectives are designed to yield an essentially perfect image, and aberrations (on axis at least) should be reduced to well below the Rayleigh limit if at all possible. Microobjectives for projection or photography may be corrected with more

448

Chapter Thirteen

Figure 13.6 Microscope objectives. (a) Low-power achro-

matic doublet or triplet. (b) 10  NA 0.25. (c) Amici objective 20  NA 0.5 to 40  NA 0.8. (d) Immersion objective. (e) Apochromatic 10  NA 0.3. Shading indicates fluorite (CaF2). (f) Apochromatic 50  NA 0.95.

emphasis on the outer portions of the field, depending on the exact application for which they are intended. These are usually ordinary achromatic doublets, or occasionally three-element systems, as shown in Fig. 13.6a. The 32mm NA 0.10 or 0.12 is the most common and produces a magnification of about 4. A 48-mm NA 0.08 is also occasionally encountered. This may be designed in exactly the same manner as the achromatic telescope objective discussed in Secs. 12.4 and 12.5, except that the “object” will be located at 150 mm (more or less) instead of at infinity. Low-power objectives.

As shown in Fig. 13.6b, these are usually composed of two widely spaced achromatic doublets. The most common objective is the 10, 16 mm, which is available in several forms. The ordinary achromatic 10 objective has an NA of 0.25 and is probably the most widely used of all objectives. The divisible or separable (Lister) version is designed so that it can be used as a 16-mm or, by removing the front doublet, as a 32-mm objective. This is accomplished at the sacrifice of astigmatism correction, since both components must be independently free from spherical and coma and thus no correction of astigmatism is possible. An apochromatic 16-mm objective is also

Medium-power objectives.

The Design of Optical Systems: Particular

449

available with an NA of 0.3; fluorite (CaF2) is used in place of crown glass to reduce the secondary spectrum. The power layout for this type of objective is usually arranged so that the product y is the same for each doublet; in this way the “work” (bending of the marginal ray) is evenly divided. Conventionally the second doublet is placed midway between the first doublet and the image formed by the first doublet. (Note that the preceding refers to raytracing sequence—in use the “second” doublet is near the object to be magnified and the “first” doublet is nearer the actual image.) This relatively large spacing allows the cemented surface of the second doublet to overcorrect the astigmatism and flatten the field (assuming the stop to be at the first doublet). This layout leads to a thin-lens arrangement with the space about equal to the focal length of the objective, the focal length of the first doublet approximately twice that of the objective, and that of the second doublet about equal to that of the objective. Note that this arrangement is similar to that of a highspeed Petzval-type projection lens (see Fig. 13.24). Ordinarily three sets of shapes for the two components can be found for which spherical and coma are corrected. One form will be that of the divisible objective, with the spherical and coma zero for each doublet; this is usually the form with the poorest field curvature. Aplanatic surfaces. If the surface contribution equation for the spher-

ical aberration of a single surface is solved for zero spherical, three solutions are found. One case occurs when the object and image are at the surface and is of little interest. A second is of more value; when object and image both lie at the center of curvature, there is no spherical aberration introduced (and the axial rays are not deviated). The third case, usually called the aplanatic case, allows the convergence of a cone of rays to be increased (or decreased) by a factor equal to the index without the introduction of spherical aberration. It occurs when any of the following relationships are satisfied.

冢

n′  n LR  n

冢

冣

冣

(13.1)

n′  n n L′  R    L n′ n′

(13.2)

U  I′

(13.3)

U′  I

(13.4)

n′ sin U′    n sin U

(13.5)

450

Chapter Thirteen

Note that if any of the above are satisfied, all are satisfied, and that, since no spherical is introduced, if L  l, then L′  l′. It is also worth noting that coma is zero for all three cases and that astigmatism is zero for the first and third cases and overcorrecting between. This principle is used in the “aplanatic front” of an oil-immersion microscope. The object is immersed in an oil whose index of refraction matches that of the first lens. R1 (as shown in Fig. 13.7) is chosen to satisfy Eq. 13.1; this results in a hyperhemispheric form for the first element. R2 is chosen so that the image formed by R1 is at its center of curvature; R3 is chosen to satisfy Eq. 13.1. Note that sin U is reduced by a factor of n at each element, and that the “aplanatic front” reduces the numerical aperture of the cone of rays from a large value (as high as NA  n sin U  1.4) to a value which a more conventional “back” system can handle. The Amici objective (Fig. 13.6c) consists of a hyperhemispheric front element combined with a Fig. 13.6b (Petzval) type of back combination. Since the Amici is usually a dry objective, the radius of the hyperhemisphere is frequently chosen somewhat flatter than that called for by the aplanatic case to partially offset the spherical introduced by the dry plano surface. The space between the hyperhemisphere and the adjacent doublet is kept small to reduce the lateral color introduced by the front element. The standard 4-mm 40 NA 0.65 to 0.85 objectives are usually Amici objectives. The working distance (object to front surface) is quite small in the Amici, to the order of a half millimeter. Since there is a direct relationship between zonal spherical and working distance in this type of objective, the higher-NA versions tend to have very short working distances. The oil-immersion objective utilizes the full “aplanatic front” and may be combined with a Fig. 13.6b type of back, as shown in Fig. 13.6d, or a more complex arrangement. Both the Amici and immersion High-power objectives.

Figure 13.7 The aplanatic front.

The object is immersed in a fluid whose index matches that of the hyperhemispheric first element. R1 is an aplanatic surface. The image formed by R1 is at the center of curvature of R2. R3 is an aplanatic surface of the same type as R1.

The Design of Optical Systems: Particular

451

types are frequently designed with fluorite (CaF2) crowns to reduce or eliminate secondary spectrum. Some of the new FK glasses can serve the same purpose. Note that although the aplanatic front is a classic textbook case, departures from the exact aplanatic form are common. For example, it is possible to find a meniscus lens of higher power than the aplanatic case which will introduce overcorrected spherical. This not only reduces the ray-bending work that the back elements must accomplish, but also reduces the correction load as regards spherical aberration (but not chromatic). Aplanatic-front objectives have a residual lateral color resulting from the separation of the chromatically undercorrected front and the overcorrecting back. Special compensating eyepieces with opposite amounts of lateral color are used to correct this situation. Flat-field microscope objectives. The objectives shown in Fig. 13.6 are

all afflicted with a strongly inward-curving field. Such objectives can yield extremely sharp images in the center of the field, but the deep field curvature and/or astigmatism severely limit the resolution toward the edge of even the relatively small field of the microscope. Many flat-field types of objectives have their Petzval curvature reduced by a thick-meniscus negative component placed in the long conjugate. This may be an achromatized doublet as shown in Fig. 13.8, or simply a thick singlet. The field-flattening effect is greater if the negative-power element or surface is a large distance from the positive-power member. Often the balance of the objective is simply a stack of positive components. The improvement in image quality at the edge of the field is quite marked when compared to the standard type of objective. Another desirable feature of this form of objective is a long working distance from object to front lens. Note that this configuration is the analog of the retrofocus or reversed telephoto camera lens. Many flat-field objectives incorporate a construction similar to the thickmeniscus doublets of the double-Gauss or Biotar form (see Fig. 13.14) as a field-flattening device. Another technique is to convert the

Figure 13.8 Achromatized negative doublet in a flat-field microscope objective.

452

Chapter Thirteen

aplanatic hemispheric or hyperhemispheric front element to a meniscus element. The concave surface is close to the object plane and acts as a “field flattener.” Its power contribution (y) is small because the marginal ray height (y) is small when close to the object plane, but the concave surface introduces a significant positive, backward-curving Petzval contribution. The commercial brand names of microscope objectives of this type usually incorporate the letters “plan” in some form. Figure 14.28 shows a high-power flat-field objective. Objectives for use in the ultraviolet or infrared spectral regions are frequently made in reflecting form, because of the difficulty of finding suitable refracting materials for these spectral regions. The central obscuration required by such a construction will modify the diffraction pattern of the image, significantly reducing the contrast of coarse targets and improving the contrast slightly for fine details, as indicated in Chap. 11. The basic construction of a reflecting objective is shown in Fig. 13.9a; it consists of two monocentric (or nearly monocentric) spherical mirrors in the Schwarzschild configuration (see Sec. 13.5). If both mirrors have a common center of curvature at the aperture stop, the system can be made free of third-order spherical, coma, and astigmatism; the focal surface is then a sphere centered on the aperture. The infinite conjugate case can be described by the following expressions (for a focal length f ): Reflecting objectives.

Space between mirrors d  2f

(13.6)

Convex radius

苶  1)f R2  (兹5

(13.7)

R1  (兹5 苶  1)f

(13.8)

Concave radius

R1-to-focus distance  ( 兹5 苶  2)f

(13.9)

苶  2)y2 y1  (兹5

(13.10)

R1 clear aperture

Fractional area obscuration  1 5

(13.11)

The Design of Optical Systems: Particular

453

Figure 13.9 Reflecting microscope objectives. (a) Concentric 30  NA 0.5. (b) Ultraviolet

50  NA 0.7. Fused quartz and calcium fluoride are used for the refracting elements. (Courtesy of D. Grey.)

There are a number of variations on this basic form, some with less obscuration, some with reduced high-order spherical aberration. The resulting system not only has zero third-order spherical, but even the higher orders tend to be exceedingly small; by proper choice of parameters, a delightfully simple but nonetheless useful objective can be obtained. The two-mirror system is limited to about 35 at NA  0.5. For higher magnifications and numerical apertures, it is necessary to introduce additional refracting elements to maintain correction, as indicated in the sketch of the 50 NA 0.7 ultraviolet objective in Fig. 13.9b. Aspheric surfaces have also been utilized. The added elements can also serve to reduce the central obscuration or to flatten the field. 13.3

Photographic Objectives

In this section, we will outline the basic design principles of the photographic objective, and for this purpose we will classify objectives according to their relationship to, or derivation from, a few major categories: (a) meniscus types, (b) Cooke triplet types, (c) Petzval types, and (d) telephoto types. These categories are quite arbitrary and are chosen for their value as illustrations of design features rather than any historic or generic implications. Meniscus anastigmats. In this category, we include those objectives

which derive their field correction primarily from the use of a thick meniscus. As mentioned in Secs. 12.1 and 12.2, a thick-meniscus element has a greatly reduced inward Petzval curvature in comparison with a biconvex element of the same power; indeed, the Petzval sum can be overcorrected if the thickness is made great enough. The simplest example of this type of lens is the Goerz Hypergon (Fig. 12.4) which consists of two symmetrical menisci. Because the convex and

454

Chapter Thirteen

concave radii are nearly equal, the Petzval sum is very small, and the fact that the surfaces are nearly concentric about the stop enables the lens to cover an extremely wide (135°) field, although at a very low aperture (f/30). To obtain an increased aperture, it is necessary to correct the spherical and chromatic aberrations. This can be accomplished by the addition of negative flint elements, as in the Topogon lens, Fig. 13.10. Note that the construction of this lens is also very nearly concentric about the stop; lenses of this type cover total fields of 75° to 90° at speeds of f/6.3 to f/11. Attempts to design a system consisting of symmetrical cemented meniscus doublets in the latter half of the nineteenth century were only partially successful. If the spherical aberration was corrected by means of a diverging (i.e., with negative power) cemented surface, the higher-order overcorrected astigmatism necessary to artificially flatten the tangential field tended to become quite large at wide angles. If a high-index crown and low-index flint were used to reduce the Petzval field curvature, the resulting collective cemented surface was incapable of correcting the spherical. In 1890, Rudolph (Zeiss) designed the Protar, Fig. 13.11, which used a low-power “old” achromat (i.e., lowindex crown, high-index flint) front component and a “new” achromat (high-index crown and low-index flint) rear component. The dispersive cemented surface of the front component was used to correct the spherical, while the collective cemented surface of the rear kept the astigmatism in control. Note that the components are thick menisci, which allows reduction of the Petzval sum, while the general

The Topogon lens (U.S. Patent 2,031,792-1936) covers 90° to 100° at a speed of f/8. Figure 13.10

The Zeiss Protar (U.S. Patent 895,045-1908). Figure 13.11

The Design of Optical Systems: Particular

455

symmetry helps to control the coma and distortion. Lenses of the Protar type cover total fields of 60° to 90° at speeds of f/8 to f/18. A few years later, Rudolph and von Hoegh (Goerz), working independently, combined the two components of the Protar into a single cemented component, which contained both the required dispersing and collective cemented surfaces. The Goerz Dagor is shown in Fig. 13.12, and is composed of a symmetrical pair of cemented triplets. Each half of such a lens can be designed to be corrected independently so that photographers were able to remove the front component to get two different focal lengths. A great variety of designs based on this principle were produced around the turn of the century, using three, four, and even five cemented elements in each component, although very little was gained from the added elements. Protars and Dagors are still used for wide-angle photography because of the fine definition obtained over a wide field, especially when used at a reduced aperture. See Fig. 14.14 for an example of a Dagor design. The additional degree of freedom gained by breaking the contact of the inside crowns of the Dagor construction proved to be of more value than additional elements. Lenses of this type (Fig. 13.13) are probably the best of the wide-angle meniscus systems and cover fields up to 70° total at speeds of f/5.6 (or faster for smaller fields). The Meyer Plasmat, the Ross W. A. Express, and the Zeiss Orthometar are of this construction, and recently excellent 1:1 copy lenses (symmetrical) have been designed for photocopy machines. Note that the broken contact allows the inner crown to be made of a higher-index glass. The design of the thick-meniscus anastigmats is a complex undertaking because of the close interrelationship of all the variables. In general the exterior shape and thickness are chosen to control the Petzval sum and power, and the distance from the stop can be used to adjust the astigmatism. However, the adjustment of element powers to correct chromatic inevitably upsets the balance, as does the bending of the entire meniscus to correct spherical. What is necessary is one simultaneous solution for the relative powers, thicknesses, bendings, and spacings; an approach of the type described in Secs. 12.7 and 12.8 for the simultaneous solution of the third-order aberrations is ideally

The Goerz Dagor (U.S. Patent 528,155,1894). The glasses used are 613:563, 568:560, and 515:547, from the left. The construction is symmetrical about the stop.

Figure 13.12

456

Chapter Thirteen

Figure 13.13 The Zeiss Orthometar (U.S. Patent 1,792,917). Constructional data and aberration curves for a focal length of 100.

suited to this problem, and the automatic computer design programs make easy work of it. The efforts of designers in this direction over the past 75 years have been well spent, and it is exceedingly difficult to improve on the best representative designs in this category unless one utilizes the newer types of optical glass (e.g., the rare earth glasses). The double-Gauss (Biotar) (Fig. 13.14) and the Sonnar types (Fig. 13.15) of objectives both make use of the thick-meniscus principle, although they differ from the preceding meniscus types in that they are used at larger apertures and smaller fields. The Biotar objective in its basic form consists of two thick negative-meniscus inner doublets and two single positive outer elements as shown in Fig. 13.14. This is an exceedingly powerful design form, and many high-performance lenses are modifications or elaborations of this type. If the vertex length is made short and the elements are strongly curved about the central stop, fairly wide fields may be covered. Conversely, a long system with flatter curves will cover a narrow field at high aperture. One possible “manual” design approach is as follows: 1. Select an appropriate vertex length, based on considerations of aperture and field coverage. Prior art is useful in this regard. Usually this length is almost filled with glass, in that the first and last airspaces

The Design of Optical Systems: Particular

457

Figure 13.14 The double-Gauss (Biotar) objective (U.S.

Patent 2,117,252-1938). Constructional data and aberration curves for a focal length of 100.

Figure 13.15 The Sonnar-type objective.

are minimal and the edge clearance between the central flints is often small. Baker, in U.S. Patent 2,532,751, suggests a rule of thumb for the total thickness of the two meniscus doublets plus the central airspace: for narrow fields (less than ±10°), a value of 0.6 to 0.7 times the focal length; for moderate fields (between ±10° and 20°), 0.5F to 0.6F; for fields larger than ±20°, a value of 0.4F to 0.5F. 2. Select glass types. Crowns are usually high-index barium or lanthanum crowns. Flints are usually lower in index by several hundredths, although higher-index flints are not uncommon. The difference in V-value can be used to shape the cemented surfaces; usually surface 4 is made concave to the stop and surface 6 convex to the stop. 3. Make a rough layout of thickness and curvature. Prior art is a useful guide. Use R5 and R6 to adjust the Petzval sum and vary R4 and R7 to correct the axial and lateral color as desired.

458

Chapter Thirteen

4. Use the third-order surface contributions to effect a solution for the desired ∑SC, ∑CC*, ∑AC*, and ∑DC*. This can be handled by plotting the contribution of each component against its shape, locating a region of solution, and applying a differential correction technique. 5. A trigonometric check and differential correction complete the primary phase of the design. 6. Note that there are many unused degrees of freedom remaining. The distribution of power from front to back elements and the distribution of power between inside and outside crowns may be systematically varied within rather broad limits. The glass and thickness choices are subject to revision as well. Each of these will have an effect on residuals and higher-order aberrations. 7. The following comments may be helpful: a. Oblique spherical (a fifth-order aberration which is characteristic of these lenses and causes spherical to vary with obliquity, i.e., as y3h2) is usually troublesome, causing an off-axis overcorrection which reduces image contrast. This comes from the large angles of incidence at surface 5 for the upper rim ray and at surface 6 for the lower. This can be reduced (at the expense of other corrections) by increasing the central airspace or by curving the system strongly about the stop to allow a more concentric passage of the rays through these surfaces, or by reducing the thickness of the doublets which will tend to force a more curved configuration on them (and also increase the zonal spherical.) Making the cemented surfaces more collective also tends to reduce the oblique spherical. Vignetting is often used to eliminate the tangential oblique spherical, but the sagittal oblique spherical cannot be vignetted out. b. The longitudinal position of surface 7 can be used to control spherochromatism. A shift to the right will reduce the spherical overcorrection of blue light relative to red light. c. If the index difference across the cemented surfaces is small, the adjustments of R4 and R7 for chromatic correction will have a correspondingly small effect on the monochromatic aberrations. d. The thickness of the cemented doublets (especially the front) has a strong effect on spherical aberration. Increasing the thickness leads to undercorrection, and vice versa. This sensitivity is a common characteristic of thick-meniscus systems which, although it makes fabrication difficult, is useful as a design tool. While the first three steps outlined above are those one might utilize in starting a double-Gauss design, steps 4, 5, and 6 can be nicely handled by an automatic design program.

The Design of Optical Systems: Particular

459

Common elaborations of the Biotar format include compounding the outer elements into doublets or triplets or converting the meniscus doublets into triplets. Frequently the outer elements are split (after shifting some power from the inner crowns) in order to increase the speed. Some recent designs have advantageously broken the contact at the cemented surface, especially in the front meniscus. One may also double up on the inner meniscus doublets. In extreme cases all the elements of the Biotar can be duplicated, leading to a 12element design with two front singlets, two front inner doublets, two rear inner doublets, and two rear singlets. Another interesting variation (the principle of which can be used in any design with a large enough airspace) is the insertion of a low- or zero-power doublet into the center airspace. The glasses of this doublet are chosen to have the same or nearly the same index and V-value, but significantly different partial dispersions. The low-power and matching index and V-value mean that the effect on most aberrations is negligible, but the partial dispersion difference can be arranged so that the secondary spectrum of the lens is reduced. There are several pairs of dense flint glasses which are suitable for this purpose. As indicated above, the double-Gauss (Biotar) is an extremely powerful and versatile design form. It is the basis of most normal focal length 35-mm camera lenses and is found in many applications where extremely high performance is required of a lens. It can be made into a wide-angle lens or can be modified to work at speeds in excess of f/1.0 with equal facility. Additional examples of double-Gauss designs are presented in Figs. 14.32, 14.33, 14.34, 14.35, and 14.36. Airspaced anastigmats. These are systems which utilize a large separation between positive and negative components to correct the Petzval sum. Although it is historically incorrect in several instances, from a design standpoint it is useful to view these lenses as derivatives from the Cooke triplet, Fig. 13.16 (see also Sec. 12.6). The Tessar (although actually derived from a meniscus-type lens) may be regarded as a triplet with the rear positive element compounded; the classic form of the Tessar is shown in Fig. 13.17. The additional freedom gained by compounding may be regarded as simply a means of artificially generating an unavailable glass type by combining two available glasses; alternatively, one may utilize the refractive characteristics of the cemented interface to control the course of the upper rim ray, which is affected strongly by this surface. The Tessar formulation, either as shown, or with the doublet reversed, or even with the front element compounded, is utilized when a performance a bit beyond that of the Cooke triplet is required. The reversed

460

Chapter Thirteen

Figure 13.16 The Cooke triplet.

Figure 13.17 The Tessar objective

(U.S. Patent 1,588,073-1922). Construction and aberration data for a focal length of 100.

doublet form is usually better when high-index rare earth glasses are utilized. Figures 14.16 and 14.17 are additional examples of Tessar designs. A further example of the compounding of the elements of the basic triplet is the Pentac (or Heliar) type, Fig. 13.18, which is simply a symmetrical extension of the Tessar principle. A Heliar design is shown in Fig. 14.18. In the Hektor (Fig. 13.19), all three elements are compounded and the speed can be raised to f/1.9 with fields to the order of ±20°. Many “compounded triplets” make use of what is sometimes called a “Merté” surface; the cemented surface of the negative component of the Hektor is an example of such a surface. This is a strongly curved (usually cemented) collective surface so arranged that the angle of incidence increases rapidly toward the margin of the lens. Such a surface contributes a modest amount of undercorrecting spherical to the rays near the axis, since the index break across the surface is not large. As the angle of incidence rises (and it may approach 45°), because of the nonlinearity of Snell’s law, the spherical aberration contribution rises even more rapidly, and

The Design of Optical Systems: Particular

461

Figure 13.18 The Pentac-Heliar anastigmat.

Figure 13.19 The Hektor anastigmat (German Patent

526,308-1930). The spherical aberration curve shows a large seventh-order component which originates at the strongly curved fifth surface: focal length, 100.

the undercorrecting effect dominates the marginal zone. The result is a spherical aberration curve which shows not only negative thirdand positive fifth-order aberration, but a sizable amount of negative seventh order as well. The spherical aberration shown in Fig. 13.19 is a rather extreme example of this technique. This is an approach which obviously must be used with discretion, since large amounts of high-order aberration are delicately balanced. Such a surface is best located near the stop to minimize the disparity of its effects on the upper versus lower rim rays; otherwise, the off-axis ray intercept curves may tend toward a very unpleasant asymmetry. A similar design is shown in Fig. 14.19.

462

Chapter Thirteen

Notice that in both Figs. 13.17 and 13.19, the doublets are composed of a positive crown with a higher index than the negative flint. The inward-curving Petzval contribution of such a doublet is much less than that of a single-lens element. And of course the undercorrected chromatic of a singlet is reduced or eliminated, since the doublet is at least partially achromatized. Remembering that the Petzval contribution is proportional to /n, it is apparent that the compounding of these elements produces a component which is equivalent to a singlet with both a high index and a high V-value. (This is true for the positive doublets; of course, the reverse is true for a negative doublet.) Note that in almost all cases where a doublet is used in an anastigmat, it is a “new achromat,” with the crown index higher than the flint index, yielding a converging cemented surface. This construction tends to have at least some of the above-mentioned “Merté” effect on the higher-order spherical, but the cemented surface does not correct the third-order spherical as the diverging cemented surface of the “old achromat” doublet does. Another basic technique for the reduction of the residual aberrations involves splitting the individual elements into two (or more) elements. A single crown element has about five times as much undercorrected spherical as a two-element lens of equivalent power and aperture when both elements are shaped for minimal spherical (see Fig. 13.53). Thus, a split allows the contributions of the other elements of the system to be reduced, resulting in a corresponding decrease in higherorder aberrations. Ordinarily the crown elements of a triplet are split when a larger aperture is desired; Figs. 13.20 and 13.21 are examples of this technique. Since it requires a fairly long system and high speed to make this technique effective, the angular coverage of such systems is usually modest. However, by compounding the split elements, excellent combinations of aperture and field have been obtained from these forms. Splitting the front crown is usually more profitable than splitting the rear, since the astigmatism at the edge of the field is better controlled in the split-front types, and the meniscus shape is beneficial for the Petzval field curvature. Although less frequently encountered, element splitting can also be effective to a limited degree in extending field coverage. Additional variants on the split-crown triplets can be found in Figs. 14.24, 14.25, 14.26, and 14.27. Split-flint triplets (Fig. 13.22) should really be regarded as thickmeniscus systems with an air lens separating the crown and flint of each half; indeed this was their historical derivation. This form is not especially notable for reduced spherical zonal as are the split-crown types, but some of the finest general-purpose photographic objectives (e.g., the f/4.5 Dogmar and Aviar lenses) have been of this construction. The general symmetry of this design lends itself to a wider angular

The Design of Optical Systems: Particular

Figure 13.20 Split-rear crown triplet (U.S. Patent

1,540,752-1924); focal length, 100.

Figure 13.21 Split-front crown triplet (English Patent

237,212-1925); focal length, 100.

463

464

Chapter Thirteen

Figure 13.22 The Dogmar anas-

tigmat (U.S. Patent 1,108,3071914); focal length, 100.

coverage than do the split-crown types, although, as in most “tripletderived” forms, the limit of coverage is often sharply defined and image quality tends to fall off rapidly beyond the stigmatic node. (This last comment is less true of systems where the crown-flint spacing is small, since these types are closer to the meniscus lenses than to triplets.) Figure 14.15 is another example of the Dogmar. Many excellent process and enlarging lenses are based on this format. Process lenses of this type can be made with glasses of unusual partial dispersions in order to correct or reduce secondary spectrum. Such lenses usually have the letters “apo” in their trade names to denote apochromatic or semiapochromatic correction. Lenses for close conjugate work, such as enlarger lenses, are often airspaced anastigmats. They differ from camera objectives primarily in that they are designed for low magnification ratios, rather than for infinite object distances. Most camera objectives maintain their correction down to object distances to the order of 25 times their focal length, and some do well at even shorter distances. Enlargers, however, are frequently used at magnifications approaching unity, and enlarging lenses are usually designed at conjugate ratios of 3, 4, or 5. A lens which is approximately symmetrical (such as the Dogmar) makes a good enlarger lens since it is a bit less sensitive to objectimage distance changes. Compounded triplets of approximately symmetrical construction are also used, and the Tessar formula is widely used because of its wide field of coverage and relatively simple and inexpensive construction.

The Design of Optical Systems: Particular

465

Petzval lenses. The original Petzval portrait lens (Fig. 13.23) was a

relatively close-coupled system consisting of two achromatic doublets, the rear doublet with broken contact, with a sizable airspace between. It covered a modest field at a speed of about f/3. The modern version, often referred to as the Petzval projection lens because of its widespread use as a motion picture projection objective, utilizes a larger airspace (almost equal to its focal length) and covers half-field of ±5° to ±10° at speeds up to f/1.6. This type of system (Fig. 13.24) is noted for the excellence of its correction on axis, and also for its strongly inward-curving field. The field is artificially flattened by overcorrected astigmatism which is introduced at the cemented surface of the rear doublet. A typical formulation has a thin-lens spacing about equal to the focal length, a front doublet with twice the focal length of the system, and a rear doublet with a focal length equal to that of the system. Thus, the (thin-lens) back focus is about half the focal length, and

Figure 13.23 The Petzval portrait lens.

Figure 13.24 The Petzval projection lens (U.S. Patent

1,843,519-1932); focal length, 100.

466

Chapter Thirteen

the front vertex-to-focal plane distance is about 1.5 times the focal length. If the airspace is appreciably shortened, it may be necessary to break contact or increase the index break at the rear doublet to maintain the overcorrected astigmatism. Note that the Petzval projection lens as shown in Fig. 13.24 is basically the same design form as that of a 10, NA 0.25 microscope objective. The Petzval projection lens construction inherently has low spherochromatism, low secondary spectrum, and a relatively small zonal spherical aberration. The inward-curving Petzval surface can be corrected by the use of a negative “field flattener” element near the focal plane, Fig. 13.25. In this location the power contribution (y) of the element is low, but the Petzval field is nicely flattened, and a lens of beautiful definition over a small field can be obtained. The drawback to this is the location of the element near the image plane, where dust and dirt can become quite noticeable. Note that the field flattener is made of flint glass, which helps the correction of the chromatic aberration.

Figure 13.25 Petzval projection lens with field flattener (U.S.

Patent 2,076,190-1937); focal length, 100.

The Design of Optical Systems: Particular

467

The glasses used in the Petzval lens are usually an ordinary crown and common dense flint. Occasionally higher-index glass is used and one or both doublets are of the broken contact type. An interesting variation on the field-flattener Petzval is shown in Fig. 13.26, in which the rear negative element does double duty, serving both as the rear flint and as the field flattener as well. The broken contact in the front doublet is necessary to correct the aberrations. This lens has a tendency toward increased zonal spherical as well as fifth-order coma of the y4h type, which is introduced by the airspaced front doublet. This aberration is frequently encountered in other design types as well, when a strong negative “air lens” is used in this manner to correct spherical aberration. The glasses used in this lens are dense barium crowns (SK4) and dense flints (SF1). The already small spherical zonal of the Petzval lens can be reduced still further by splitting the rear doublet into two doublets as indicated in Fig. 13.27 or by the introduction of a meniscus element into the central airspace, Fig. 13.28. One Petzval modification achieved a speed of f/1.0 (with an almost spherical image surface) by splitting off a sizable part of the power of each crown element into separate planoconvex elements. Other modifications have made use of strongly meniscus front correctors to reduce the spherical zonal, or of thick rear concentric meniscus elements to improve the field. Two recent designs which are used as 2-in f/1.4 projection lenses for 16-mm motion pictures are shown in Fig. 13.29. Additional variations on the Petzval theme are shown in Figs. 14.20, 14.21, 14.22, and 14.23. Telephoto lenses. Telephoto lenses are arbitrarily defined as lenses whose length from front vertex to film plane is less than the focal length. The telephoto ratio is the vertex length divided by the focal length; a lens with a ratio of one or less is considered a telephoto lens. This is achieved by a positive front component separated from a

Figure 13.26 f/1.6 Petzval lens with field-flattening effect achieved by large airspace between rear crown and flint.

Figure 13.27 f/1.3 Petzval lens

with two rear doublets to reduce spherical zonal. (U.S. Patent 2,158,202-1939).

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Chapter Thirteen

13.28 Field-flattener Petzval lens with front crown split into two elements to reduce spherical zonal. (U.S. Patent 2,541,484-1951).

Figure

Figure 13.29 High-performance 2-in, f/1. 4, 16-mm motion picture projection

lenses. (Left is U.S. Patent 2,989,895-1961. Right is U.S. Patent 3,255,6641966).

negative rear component, as indicated in Fig. 13.30. Several forms of telephoto lenses are also shown; distortion correction is usually achieved by splitting the rear component. A common difficulty of the telephoto and reverse telephoto lenses is a strong inclination toward an overcorrected Petzval sum and a backward-curving field when extreme ratios are obtained. Figure 14.13 shows a typical telephoto lens design. Reverse telephoto (retrofocus) lenses. By reversing the basic power

arrangement of the telephoto, a back focal length which is longer than the effective focal length may be achieved. This (Fig. 13.31) is a useful form when prisms or mirrors are necessary between the lens and the image plane; it also allows the use of a short-focallength projection lens with a condenser designed for longer lenses, since the pupil position is well away from the image plane. The construction was originally a strong negative achromat in front, combined with a modification of a standard objective. Biotars, triplets, and Petzvals have all been used for the rear member. It is usually necessary to split the negative achromat and bend it concave to the rear member to achieve good correction. In extreme forms (“skylenses” or “fish-eye” lenses) coverage can exceed ±90° with a very strongly meniscus negative front element. Obviously in order to image 180° or more on a finite-sized flat film, a large amount of distortion is unavoidable. The retrofocus lens has found wide use with the popularity of the single-lens reflex 35-mm camera, which requires a long back focus to clear the viewfinder mirror as it swings up out of the way when the exposure is made. All of the short-focus, wide-angle SLR lenses are of

The Design of Optical Systems: Particular

469

Figure 13.30 Telephoto lenses. A focal length

which is greater than the physical length of the lens is achieved by a positive front member widely separated from a negative rear member.

Figure 13.31 The reverse telephoto is characterized by a long back

focus which is useful for short-focal-length lenses. In extreme forms (right-hand sketch) the coverage can be made to exceed 180°.

this type. The retrofocus has evolved into a very powerful design form in its own right and can no longer be regarded as a standard camera lens with a negative lens out in front. After all, since the front negative component more than corrects the Petzval curvature, it makes little sense to overdo the correction with an already field-flattened standard design type. Figures 14.11 and 14.12 show a retrofocus and a “fish-eye” lens, respectively.

470

Chapter Thirteen

If one examines the ray path in the right-hand sketch of Fig. 13.31, it is apparent that the negative element is reducing the angular coverage required of the positive element. This idea is the basis of many wide-angle camera lenses; this type consists of a collection of positive components surrounded by meniscus negative elements. The Angulon and several other designs are of this type. Figures 14.37 and 14.38 show examples of this type of wide-angle lens. These usually take the form of Galilean or reversed-Galilean telescopes as indicated in Fig. 13.32. The focal length of the “prime” lens is multiplied by the magnification of the telescopic attachment. The field of view limits the power of the telephoto types to about 1.5, but the wide-angle type of attachment is useful to about 0.5. Such systems are, of course, designed to use an external stop (that of the prime lens) and frequently require quite a bit of “stopping-down” to achieve satisfactory imagery, especially in the simpler constructions. An afocal attachment can be added to almost any optical system in order to change its focal length or field or magnification. The idea is obviously most applicable where the object or image is at a distance so that the afocal is working in collimated light. For noncollimated applications a Bravais system (see Sec. 9.9) can serve the same function. Afocal attachments.

13.4

Condenser Systems

The condenser in a projection system is quite analogous to the field lens in a telescope or radiometer. The function of the condenser is illus-

Figure 13.32 The focal length of a prime lens can be modified by the use of an

afocal attachment, which is basically a Galilean telescope. The upper sketch shows a “telephoto” attachment which increases the focal length. The lower system is a “wide-angle” which reduces the focal length.

The Design of Optical Systems: Particular

471

Figure 13.33 The projection condenser produces an image of

the source in the pupil of the projection lens. Note that the minimum condenser diameter for optimum illumination at the image of point C is determined by a line through C and the opposite rim of the pupil.

trated in Fig. 13.33. The upper sketch shows a projection system without a condenser. It is apparent that for the axial object point A, only about half the lens area can be used, for point B only an even smaller fraction of the lens is utilized, and that no light from the lamp passing through point C can pass through the projection lens. The result is that the illumination at the projected image is not as high as it might be and drops off rapidly away from the axis. This can be alleviated somewhat by moving the lamp closer to the film, and, in a very few cases, this solution is satisfactory, if inefficient. However, the filament is usually not uniform enough to allow it to be projected directly without producing objectionable nonuniformity of illumination at the image. The “Koehler” projection condenser shown in the lower sketch of Fig. 13.33 images the lamp filament directly into the aperture of the projection lens. If the image size is equal to (or greater than) the lens aperture size, the illumination is optimized, and if the condenser has a sufficient diameter, the illumination over the full image field is as uniform as possible. The requirements for an ideal condenser may be expressed as follows: The image of the filament must completely fill the projection lens aperture through a small pinhole placed anywhere in the field (i.e., at the film plane). The photometric aspects of condensers are discussed in Sec. 8.10.

472

Chapter Thirteen

The chief aberrations of concern in condenser systems are usually spherical and chromatic aberrations; coma, field curvature, astigmatism, and distortion are of secondary importance in ordinary systems. Figure 13.34 is an exaggerated sketch of a condenser afflicted with spherical aberration. Note that the filament image formed by the marginal zone of the condenser completely misses the projection lens aperture, resulting in a marked falloff in illumination at the edge of the field. This situation could be alleviated by reducing the condenser power so that the marginal ray focus was at the lens; however, in difficult cases this can result in a dark zonal ring in the field because at least some of the zonal rays will then miss the aperture. The effects of chromatic aberration are similar, except that one end of the spectrum (red or blue) may miss the aperture and cause an unevenly colored field of view, especially noticeable at the field boundary. Except in unusual cases (e.g., some microscope condensers) chromatic effects can be held to a tolerable level without achromatizing. Spherical aberration is controlled by splitting the condenser into two or three elements of approximately equal power and bending each element toward the “minimum spherical” shape, as indicated in Fig. 13.35a and b. An aspheric surface can be molded on one of the elements to reduce the spherical aberration, as in Fig. 13.34c. The aspheric is often a simple paraboloid, and a molded surface can be sufficiently precise to meet the requirements of a condenser system. When the light source is uniformly bright, it can be imaged directly on the film gate. In arc-lamp motion picture projectors, an ellipsoidal mirror is used for this purpose, as shown in Fig. 13.35d. Note that for full illumination the mirror must be large enough to accept the ray from the bottom of the projection lens aperture through the top of the film gate, just as in the Koehler condenser. The ellipsoidal mirror is used since it has no spherical aberration when the arc is at one focus of the ellipse and the image (film gate) is at the other. Note that an ellipsoid does have a substantial coma, however, and thus off-axis

Figure 13.34 Spherical aberration in a condenser can

cause the rays through the margin of the condenser to completely miss the aperture of the projection lens.

The Design of Optical Systems: Particular

473

Condensing systems. (a) Two-element design with reflector concentric to source. (b) Three elements, shaped to minimize spherical. (c) Aspheric surfaces can be used to reduce spherical. (d) The crater of a carbon arc can be imaged directly at the film gate by an ellipsoidal mirror.

Figure 13.35

imagery through the margin of the mirror may depart considerably from that predicted by first-order optics. Some projection lamps incorporate a reflector inside the glass bulb which functions in the same manner as the ellipsoidal mirror of Fig. 13.35d. This allows the system to push the limits on the smallness of the source (as described in Sec. 8.10) and makes for efficient usage of a small, low-wattage lamp filament. The mirrors in this type of projection lamp are often facetted; this allows some control over the magnification produced by each zone of the reflector, and also allows the direction in which the light is reflected to be adjusted in order to provide the most desirable distribution in the film gate. Another construction uses a small lamp integrally fabricated with a molded, faceted, and much larger reflector. The lamp filament is located close to the focal point of the reflector, and the condenser images the entire reflector in the projection lens aperture in what is effectively a Koehler configuration, treating the entire reflector as the source. Most condensing systems can be significantly improved by the addition of a spherical reflector behind the light source, as indicated in Fig. 13.35a. If the source is at the center of curvature, the mirror images the source back on itself, effectively increasing its average brightness. With a lamp filament of relatively open construction, such as a V

474

Chapter Thirteen

shape, or two parallel coils, the increase in illumination may approach the reflectivity of the reflector, i.e., 80 to 90 percent. The gain is much less in a tightly packed source, but even a biplane filament will gain 5 or 10 percent from a properly aligned reflector. It should be noted that if the projection lens aperture is only partially filled by the filament image, the diffraction effects will differ from those associated with a fully illuminated aperture. For example, if only the center of the aperture is illuminated, this “semicoherent illumination” causes the MTF at low frequencies to be increased, and the MTF at high frequencies to be reduced. If a two-coil filament is imaged with the coil images at the extreme edges of the aperture and the center unilluminated, not only is the MTF balance between high and low frequencies changed, but the imagery in one meridian (i.e., line orientation) is quite different from that in the other, often giving the impression of an astigmatic image. 13.5

Reflecting Systems

The increasing use of optical systems in the nonvisual regions of the spectrum, i.e., the ultraviolet and infrared regions, has resulted in a corresponding increase in the use of reflecting optics. This is due primarily to the difficulty in procuring completely satisfactory refractive materials for these regions, and secondarily, to the fact that many of the applications permit the use of relatively unsophisticated mirror systems. The material difficulty is of two kinds. Many applications require the use of a broad spectral band, and a refractive material must transmit well over the full band to be of value. Secondly, chromatic aberration can be difficult to correct over a wide spectral band, and the residual secondary spectrum is sometimes intolerable. A review of Chap. 7 will demonstrate quite clearly the advantages of a reflector in this regard; an ordinary aluminized mirror actually has much better reflectance in the infrared than in the visible and (with special attention) aluminum mirrors suitable for the ultraviolet can be fabricated. Pure reflecting systems are, of course, completely free of chromatic aberration over any desired bandwidth. The spherical mirror. The simplest reflecting objective is the spherical

mirror. For distant objects the spherical mirror has undercorrected spherical aberration, but the aberration is only one-eighth of that of an equivalent glass lens at “minimum bending.” The sphere is an especially interesting system when the aperture stop is located at the center of curvature, as shown in Fig. 13.36, because the system is then monocentric, and any line through the center of the stop may be

The Design of Optical Systems: Particular

475

Figure 13.36 A spherical reflec-

tor with the stop at its center of curvature forms its image on a concentric spherical focal surface. The image is free of coma and astigmatism when the stop is at this position.

considered to be the optical axis. The image quality is thus practically uniform for any angle of obliquity and the only aberration present is spherical aberration. Coma and astigmatism are zero, and the image surface is a sphere of radius approximately equal to the focal length, centered about the center of curvature. We can approximate the spherical aberration by use of the third-order surface contribution equations. Setting n  n′  1.0 in Eq. 10.7g, we find that y2 SC   4R

(m  1)2 SC   y2 4R

冤

冥

(13.12)

where y is the semiaperture, R is the radius, and m is the magnification. The first expression applies for an infinite object distance, and the bracketed expression applies to finite conjugates. Using Eq. 11.21 to determine the minimum diameter of the blur spot B, we find that y3 B  2 4R

(m  1)2y3 B   (m  1)4R2

冤

冥

(13.13)

This expression can be converted into the angular blur (in radians) by dividing by the image distance l′ (or focal length) to get y3   3 2R

(m  1)2y3    (m  1)2 2R3

冤

冥

(13.14)

By substituting f  R/2 and (f/#)  f/2y  R/4y  relative aperture or NA  2y/R, we obtain the following convenient expression for the angular blur size of a spherical mirror as a function of its speed (for infinite object distance) 1 NA3 0.00781      radians 3   3 128(f/#) (f/#) 16

(13.15)

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Chapter Thirteen

Although this is exact only for the third-order spherical, the expression is quite reliable up to speeds of f/2. At f/1 the exact ray-traced value of  is 0.0091, at f/0.75 it is about 0.024, and at f/0.5 it is about 0.13 radians. When the stop is not at the center of curvature, coma and astigmatism are present, and (for an infinite object distance) the third-order contributions are (R  lp) up y2 (R  lp) up CC*     2 32 (f/#)2 2R

(13.16)

(lp  R)2 up2 AC*   4R

(13.17)

up2 R h2 PC     4 2f

(13.18)

where up is the half-field angle and lp is the mirror-to-stop distance. Note that when lp is equal to R, CC* (the sagittal coma) and AC* (onehalf the separation of the S and T fields) are zero. For the case of the stop located at the mirror, we find the minimum angular blur sizes to be Comas: up   2 radians 16 (f/#)

(13.19)

Compromise focus astigmatism: up2    radians 2 (f/#)

(13.20)

Equations 13.15, 13.19, and 13.20 provide a very convenient way of estimating the image size for a spherical mirror when combined with the knowledge that (1) coma and astigmatism are zero with the stop at the center of curvature and (2) coma varies linearly (per Eq. 13.16) and astigmatism varies quadratically (per Eq. 13.17) with the distance of the stop from the center of curvature. The sum of the spherical, coma, and astigmatism blur angles gives a fair estimate of the effective size of a point image for a spherical mirror. The paraboloidal reflector. Reflecting surfaces generated by rotation of the conic sections (circle, parabola, hyperbola, and ellipse) share two valuable optical properties. First, a point object located at one focus is imaged at the other focus without spherical aberration. The paraboloid of revolution, Fig. 13.37, described by the equation

The Design of Optical Systems: Particular

477

(a) A parabolic reflector is free of astigmatism when the stop is at the focus. (b) The Herschel mount for a paraboloid uses an off-axis aperture to keep the focus out of the entering beam. (c) The newtonian mount utilizes a 45° plano reflector to direct the focus to an accessible point outside the main tube of the telescope.

Figure 13.37

y2 x  4f

(13.21)

has one focus at f and the other at infinity, and is thus capable of forming perfect (diffraction limited) images of distant axial objects. The second characteristic of a conicoid is that if the aperture stop is located at the plane of a focus, as for example in Fig. 13.37a, then the image is free of astigmatism. However, the paraboloid is not completely free of aberrations; it has both coma and astigmatism. Since it has no spherical aberration, the position of the stop does not change the amount of coma, which is given by Eq. 13.19. The amount of astigmatism is modified by the stop position. With the stop at the mirror the astigmatism is given by Eq. 13.20; when the stop is at the focal plane, the astigmatism is zero and the image is located on an approximately spherical surface of radius f, as shown in Fig. 13.37a. The imaging properties of these conic sections are made use of in the Gregorian and Cassegrain telescopic systems, as indicated in Figs. 13.38 and 13.39, respectively. The primary mirror in each of these is a paraboloid which produces an aberration-free axial image at its focus. The secondary mirror is located so that its first focus coincides with the focus of the paraboloid. The ellipsoid and hyperboloid.

478

Chapter Thirteen

Upper: A point object at one focus of an elliptical reflector is imaged at the other focus without spherical aberration. Lower: The classical Gregorian telescope uses a parabolic primary mirror and an elliptical secondary so that the image is free of spherical.

Figure 13.38

Figure 13.39 Upper: A ray direct-

ed toward one focus of a hyperbola is reflected through the other focus. Lower: The classical Cassegrain objective uses a parabolic primary mirror with a hyperboloid secondary. When the primary image is at the focus of the secondary mirror, the final image has no spherical aberration. If the osculating radii of the surfaces are equal, the Petzval field is flat.

Thus the final image is located at the second focus of the secondary mirror and is completely free of spherical aberration. The paraboloid, ellipsoid, and hyperboloid all suffer from coma (compare the magnification produced by the dotted versus the solid lines in Fig. 13.38) and astigmatism, so that the image is aberration-free only exactly on the axis. It should be apparent that either the Gregorian or Cassegrain objective systems could be made up with almost any arbitrary (within reason) surface of rotation for the primary mirror; some surface then could be found for the secondary mirror which would produce a spherical-free image. This is, in effect, an extra degree of freedom which can be used by the designer to improve the off-axis imagery of these systems.

The Design of Optical Systems: Particular

479

The Ritchey-Chretien objective uses this extra degree of freedom to correct both spherical and coma simultaneously in the Cassegrain configuration. Both mirrors are hyperboloids. The same idea can be applied to the Gregorian or any other two-mirror configuration. The third-order aberration surface contribution equations (Eqs. 10.7) can be used to evaluate the aberrations of a system of two mirrors. The following equations apply to any two-mirror system, regardless of configuration. The curvatures of the primary and secondary mirrors are given by (B  F) C1   2DF (B  D  F) C2   2DB where F is the effective focal length of the combination, B is the back focus (i.e., the distance from mirror #2 to the focus), and D is the spacing between mirrors (the sign of D is here taken as positive). Note that any configuration can be obtained by suitably choosing F, B, and D. The Cassegrain has a positive focal length, the Gregorian a negative one. Both have a focal length which is long compared to D. The Schwarzschild (see Fig. 13.9) configuration results if B is chosen long compared with D. If we assume an object at infinity and place the stop at the primary mirror, the third-order aberration sums are given by ∑TSC  Y 3 [F (BF)3  64D3F 4K1  B (FDB) (F  DB)2  64B4D3K2]  8D 3F 3 ∑CC  HY 2 [2F (BF)2  (FDB) (F  DB) (DFB) 64B3D3K2]  8D2F 3 H 2Y [4BF (B  F)  (F  D  B) (D  F  B)2  64B 3D 3K2] ∑TAC   8BDF 3 H 2Y [DF  (B  F)2] ∑TPC   2BDF 2 where Y  the semiaperture of the system H  the image height B  distance from mirror #2 to image (i.e., the back focal length)

480

Chapter Thirteen

F  system focal length D  spacing (use positive sign) ∑TSC  transverse third-order spherical aberration sum ∑CC  third-order sagittal coma sum ∑TAC  transverse third-order astigmatism sum ∑TPC  transverse Petzval curvature sum and where K1 and K2 are the equivalent fourth-order deformation coefficients for the primary and secondary mirrors. For a conic section, K is equal to the conic constant " (kappa) divided by 8 times the cube of the surface radius. Thus K  "/8R3 and "  8KR3 We can readily solve for the standard design forms. If both mirrors are independently corrected for spherical aberration, we get the classical Cassegrain or Gregorian, and (F  B)3 K1   64D 3F 3 (F  D  B) (F  D  B)2 K2   64B3D3 ∑TSC  0.0 HY 2 ∑CC   4F 2 H 2Y (D  F) ∑TAC   2BF 2 Note that the coma is a function of only the field (H) and the NA; B and D do not enter. All Cassegrains and Gregorians have the same thirdorder coma. For a Ritchey-Chretien, we can solve for K1 and K2 to get both thirdorder spherical and coma corrected, and [2BD2  (B  F)3] K1   64D3F3 [2F (B  F)2  (F  D  B) (F  DB) (D  F  B) ] K2   64B3D3 ∑TSC  0.0 ∑CC  0.0 H 2Y (D  2F) ∑TAC   4BF 2

The Design of Optical Systems: Particular

481

A Dall-Kirkham system has a spherical secondary, and all of the correction is accomplished by the aspheric primary. Thus [F (F  B)3  B (F  D  B) (F  D  B)2] K1   64D3F 4 K2  0.0 ∑TSC  0.0 ∑CC 

HY 2 [2F (BF)2  (FDB) (F  DB) (DFB)]  8D2F 3

H 2Y [4BF (B  F)  (F  D  B) (D  F  B)2] ∑TAC   8DBF 3 A sort of inverse Dall-Kirkham has a spherical primary and an aspheric secondary: K1  0.0 [F (B  F)3  B (F  D  B) (F  D  B)2] K2   64B 4D 3 ∑TSC  0.0 HY 2 [2BD 2  (B  F) 3] ∑CC   8BD 2F 2 H 2Y [ (F  B) 3  4BD (D  F)] ∑TAC   8B 2DF 2 These expressions, as mentioned above, are perfectly general, and apply to any and all two-mirror systems. They are of course limited to the third order, but are surprisingly accurate up to a speed of f/2.5 or f/3. One can use these results as starting forms for the development of faster or more complex designs, incorporating an aspheric corrector plate or a third mirror to achieve additional correction of, for example, astigmatism. The results of these expressions make excellent starting designs for higher-speed systems. Note that the conics may appear to violate the principles of image illumination laid down in Chap. 8. For example, a paraboloid can readily be constructed with a diameter more than twice its focal length; a paraboloid with a speed of say f/0.25 is quite feasible and will indeed be free of spherical aberration on the axis, whereas in preceding

482

Chapter Thirteen

chapters, we may have led the reader to believe that a speed of f/0.5 was the largest aperture attainable. This apparent paradox can be resolved by an examination of Fig. 13.40 which shows an f/0.25 parabola. Note that the focal length is equal to f only for the axial zone and that for marginal zones the focal length is much larger; for marginal zones the effective focal length of a parabola is given by y2 Ffxf  4f

(13.22)

The parabola is thus far from an aplanatic (spherical- and coma-free) system. For an f/0.25 paraboloid the marginal zone focal length is twice that of the paraxial zone and the magnification is correspondingly larger. Thus, if the object has a finite size, the image formed by the marginal zones of this mirror will be twice as large as those from the axial zone; this is, of course, nothing but ordinary coma (the “variation of magnification with aperture”). The parabola is thus aberration-free only exactly on the axis. The apparent contradiction of our image illumination principles is thus resolved since we had assumed aplanatic systems in their derivations. From another viewpoint, we can remember that although the parabola forms a perfect image of an infinitesimal (geometrical) point, such a point (being infinitesimal) cannot emit a real amount of energy; the moment one increases the object size to any real dimension, the parabola has a real field, the image becomes comatic, and the energy in the image is spread out over a finite blur spot. This reduces the image illumination to that indicated as the maximum in Chap. 8. The Cassegrain objective system is used (usually in a modified form) in a great variety of applications because of its compactness and the

13.40 Illustrating the extreme variation of focal length with ray height in an f/0.25 parabolic reflector.

Figure

The Design of Optical Systems: Particular

483

fact that the second reflection places the image behind the primary mirror where it is readily accessible. It suffers from a very serious drawback when an appreciable field of view is required, in that an extreme amount of baffling is necessary to prevent stray radiation from flooding the image area. Figure 13.41 indicates this difficulty and the type of baffles frequently used to overcome this problem. An exterior “sunshade,” which is an extension of the main exterior tube of the scope, is frequently used in addition to the internal baffles. Because of their uniaxial character, aspheric surfaces are much more difficult to fabricate than ordinary spherical surfaces. A strong paraboloid may cost an order of magnitude more than the equivalent sphere; ellipsoids and hyperboloids are a bit more difficult, and nonconic aspherics are more difficult still. Thus one might well think twice (or three times) before specifying an aspheric. Often a spherical system can be found which will do nearly as well at a fraction of the cost. This is also true in refracting systems of moderate size where several ordinary spherical elements can be purchased for the cost of a single aspheric. For very large one-of-a-kind systems, however, aspherics are frequently a sound choice. This is because the large systems (e.g., astronomical objectives) are, in the final analysis, handmade, and the aspheric surface adds only a little to the optician’s task. Computer-controlled single-point diamond machining has become a practical technique for fabricating aspheric surfaces. While this is especially true for infrared optics, aspheric surfaces which owe their feasibility to diamond turning are showing up in many commercial applications such as high-level photographic optics. Extremely stable and precise machine tools (e.g., lathes, mills) can produce surfaces with turning marks which are small enough to allow their use in highquality optical systems. A limitation on diamond turning is that there is only a small number of materials which can be diamond turned. Included are germanium, silicon, aluminum, copper, nickel, zinc sulfide, selenide, and plastics. Note that glass and ferrous metals are not included in this list. However, glass molding techniques have reached

Complex conical baffles are necessary in a Cassegrain objective to prevent stray radiation from flooding the image plane.

Figure 13.41

484

Chapter Thirteen

a quality level that permits the molding of aspheric surfaces which are usable in diffraction-limited systems. For example, both molded glass and plastic aspheric lenses are made for laser disk objectives. The precision molds for these processes are made on computer-controlled equipment, and in some cases they are also diamond turned. Conic section through the origin.

Where r is the radius (at the axis) and

c is the curvature (c  1/r). y2  2rx  px2  0 r± 兹苶 r2  p苶 y2 cy2 x     p 1  兹苶 1  p苶 c2y2 y2 2r

1 py4 2 2!r

1 3 p2y6 2 3!r

1 3 5 p3y8 2 4!r

1 3 5 7 p4y10 2 5!r

x           ... 5 9 3 5 4 7 2 3

Ellipse

p1

conic constant kappa  p  1

Circle

p1

苶 conic eccentricity e  兹1p

Ellipse

1p0

Parabola

p0

Hyperbola

p0

Distance to foci: r  (1± 兹苶 1p ) p Magnification: 1  兹苶 1p   1  兹苶 1p

冤

Intersects axis at:

冥

2r x  0,  p Distance between conic and a circle of the same vertex radius r (i.e., departure from a sphere): 1 3 (p2  1) y6 1 3 5 (p3  1) y8 (p  1) y4  

x      ... 2 33! r5 2 44! r7 222! r3 Angle between the normal to the conic and the x axis:

冤

冥

y   tan1  (r  px)

The Design of Optical Systems: Particular

485

y sin    [y2  (r  px)2]1/2 Radius of curvature: Meridional:

[y2  (r  px)2]3/2 Rs3  Rt    r2 r2

Sagittal (distance to axis along the surface normal): Rs  [y 2  (r  px) 2]1/2 The Schmidt system. The Schmidt objective (Fig. 13.42) can be viewed

as an attempt to combine the wide uniform image field of the stop-atthe-center sphere with the “perfect” imagery of the paraboloid. In the Schmidt, the reflector is a sphere and the spherical aberration is corrected by a thin refracting aspheric plate at the center of curvature. Thus the concentric character of the sphere is preserved in great measure, while the spherical aberration is completely eliminated (at least for one wavelength). The aberrations remaining are chromatic variation of spherical aberration and certain higher-order forms of astigmatism or oblique spherical which result from the fact that the off-axis ray bundles do not strike the corrector at the same angle as do the on-axis bundles. The action of a given zone of the corrector is analogous to that of a thin refracting prism. For the on-axis bundle, the prism is near minimum deviation; as the angle of incidence changes, the deviation of the “prism” is increased, introducing overcorrected spherical. Since the action is different in the tangential plane than in the sagittal plane, astigmatism results. This combination is oblique spherical aberration. The meridional angular blur of a Schmidt system is well approximated by the expression

Figure 13.42 The Schmidt sys-

tem consists of a spherical reflector with an aspheric corrector plate at its center of curvature. The aspheric surface in the f/1 system shown here is greatly exaggerated.

486

Chapter Thirteen

up2   3 radians 48 (f/#)

(13.23)

There are obviously an infinite number of aspheric surfaces which may be used on the corrector plate. If the focus is maintained at the paraxial focus of the mirror, the paraxial power of the corrector is zero and it takes the form of a weak concave surface. The best forms have the shape indicated in Fig. 13.42, with a convex paraxial region and the minimum thickness at the 0.866 or 0.707 zone, depending on whether it is desired to minimize spherochromatic aberration or to minimize the material to be ground away in fabrication. The performance of the Schmidt can be improved slightly by (1) incompletely correcting the axial spherical to compensate for the off-axis overcorrection, (2) “bending” the corrector slightly, (3) reducing the spacing, (4) using a slightly aspheric primary to reduce the load on, and thus the overcorrection introduced by, the corrector. Further improvements have been made by using more than one corrector and by using an achromatized corrector. A near-optimal corrector plate has a surface shape given by the equation z  0.5Cy2  Ky4  Ly6 where 3 C  2 128 (n  1) f (f/#)

冤

冥

2 3 1  2 64 (f/#) K   32 (1  n) f 3 1 L  5 85.8 (1  n) f

and f is the focal length, f/# is the speed or f-number, and n is the index of the corrector plate. The aspheric corrector of the Schmidt is usually easier to fabricate than is the aspheric surface of the paraboloid reflector. This is because the index difference across the glass corrector surface is about 0.5 compared to the effective index difference of 2.0 at the reflecting surface of the paraboloid, making it only one-fourth as sensitive to fabrication errors. An aspheric corrector plate of this type can be added to most optical systems. One must remember that an aspheric surface placed at the aperture stop (as in the Schmidt system) will affect only the spherical aberration and that the aspheric must be placed well away from the

The Design of Optical Systems: Particular

487

stop if it is to be used to correct coma or astigmatism. An aspheric plate can be added to any of the two-mirror systems described in previous sections; if both mirrors are aspheric, the addition of the corrector plate provides enough degrees of freedom to correct spherical, coma, and astigmatism. Corrector plates have been used in the entrance beam or in the image space. An example is the “Schmidt Cassegrain,” where both mirrors of the Cassegrain configuration are simple spheres. The aspheric corrector plate is the front window of the system and is often used to support the secondary mirror. This is an economical and commercially successful system. The Mangin mirror. The Mangin mirror is perhaps the simplest of the

catadioptric (i.e., combined reflecting and refracting) systems. It consists of a second-surface spherical mirror with the power of the first surface chosen to correct the spherical aberration of the reflecting surface. Figure 13.43 shows a Mangin mirror. The design of a Mangin is straightforward. One radius is chosen arbitrarily (a value about 1.6 times the desired focal length is suitable for the reflector surface) and the other radius is varied systematically until the spherical aberration is corrected. The correction is exact for only one zone, however, and an undercorrected zonal residual remains. The size of the angular blur spot resulting from the zonal spherical can be approximated (for apertures smaller than about f/1.0) by the empirical expression 103   4 radians 4 (f/#)

(13.24)

Note that this is the minimum-diameter blur and that the “hard-core” blur diameter is smaller, as discussed in Chap. 11. At larger apertures, the angular blur predicted by Eq. 13.24 is too small; for example, at f/0.7 the blur is about 0.002 radians, almost twice as large as that predicted by Eq. 13.24. Since the Mangin is roughly equivalent to an achromatic reflector plus a pair of simple negative lenses, the system has a very large overcorrected chromatic aberration. This can be corrected by making an achromatic doublet out of the refracting element. For the simple Mangin, the chromatic angular blur is approximated by 1    radians 6V (f/#)

(13.25)

where V is the Abbe V-value of the material used. Note that this is only about one-third of the chromatic of a simple lens. The coma blur of the Mangin primary mirror is approximately onehalf of that given by Eq. 13.19. Since the spherical aberration is corrected, little change in the coma results from a shift of the stop position.

488

Chapter Thirteen

Figure 13.43 In the Mangin mirror (left) the spherical aberration of the sec-

ond surface reflector is corrected by the refracting first surface. In the righthand sketch, the spherical is corrected by a Mangin-type secondary. The dotted lines indicate the manner in which color correction can be achieved. In a doublet Mangin, glass choice can be used as a design freedom.

The Mangin principle may be applied to the secondary mirror of a system as well as to the primary. The right-hand sketch of Fig. 13.43 shows a Cassegrain type of system in which the secondary is an achromatic Mangin mirror. Such a system is relatively economical and light in weight, since all surfaces are spheres and only the small secondary needs to be made of high-quality optical material. The power of a thin second-surface reflecting element is given by   2C1 (n  1)  2C2n The Mangin mirror is often used as an element of a more complex system. For example, the primary or secondary of a system may be a Mangin; as such, it serves to correct aberrations without adding significantly to the weight of the system and often effectively replaces an expensive aspheric surface. The Bouwers (Maksutov) system. The Bouwers (or Maksutov) system

may be considered a logical extension of the Mangin mirror principle in which the correcting lens is separated from the mirror to allow two additional degrees of freedom, producing a great improvement in the image quality of the system. A popular version of this device is the Bouwers concentric system, shown in Fig. 13.44. In this system, all surfaces are made concentric to the aperture stop, which (as we have noted in the case of the simple spherical mirror) results in a system with uniform image quality over the entire field of view. This is an exceedingly simple system to design, since there are only three degrees of freedom, namely, the three curvatures. One chooses R1 to set the scale of the lens (a value of R1 equal to about 85 percent of the intended focal length is appropriate) and R2 to provide an appropriate thickness for the corrector, and then determines the value of R3 for which the marginal spherical is zero. Because of the mono-

The Design of Optical Systems: Particular

489

centric construction, coma and astigmatism are zero, and the image is located on a spherical surface which is also concentric to the stop and whose radius equals the focal length of the system. Thus only a few rays need be traced to completely determine the correction of the system. One of the interesting features of this system is that the concentric corrector element may be inserted anywhere in the system (as long as it remains concentric) and it will produce exactly the same image correction. Two equivalent positions for the corrector are shown in Fig. 13.44. A third position is in the convergent beam, between the mirror and the image. If we accept the curved focal plane, the only aberrations of the Bouwers concentric system are residual zonal spherical aberration and longitudinal (axial) chromatic aberration. In general, as the corrector thickness is increased, the zonal is reduced and the chromatic is increased. The concentric system described above is used for most applications requiring a wide field of view. When the field requirements permit, the zonal spherical or the chromatic may be reduced by departing from the concentric mode of construction, although this is, of course, accomplished at the expense of the coma and astigmatism correction. If one of the thick-lens equations (Eq. 2.36 or 2.37) is differentiated with respect to the index, the result can be set equal to zero and the equation solved for the shape of an element whose power or image distance does not vary with a change in index (or a change in wavelength). This is an achromatic singlet. It takes the shape of a thick meniscus element, and this can be used as an achromatic corrector, just as in Fig. 13.44. This is the basis of the Maksutov system.

Figure 13.44 In the Bouwers concentric catadioptric sys-

tem, all the surfaces are concentric about the aperture. The “front” and “rear” versions of the corrector are identical and produce identical correction. The rear system is more compact, but the front system can be better corrected, since it can utilize a greater corrector thickness without interference with the focal surface. Occasionally, correctors in both locations are utilized simultaneously.

490

Chapter Thirteen

Another means of effecting chromatic correction is shown in Fig. 13.45a, in which the corrector meniscus is made achromatic. Note that concentricity is destroyed by this technique, although if the crown and flint elements are made of materials with the same index but different V-values (e.g., DBC-2, 617:549, and DF-2, 617:366), the concentricity can be preserved for the wavelength at which the indices match, and only the chromatic correction will vary with obliquity. A very powerful system results if the concentric Bouwers system is combined with a Schmidt-type aspheric corrector plate, as shown in Fig. 13.45b. Since the aspheric plate need only correct the small zonal residual of the concentric system, its effects are relatively weak and the variation of effects with obliquity are correspondingly small. The Baker-Nunn satellite tracking cameras are based on this principle, although their construction is more elaborate, using doublemeniscus correctors and three (achromatized) aspheric correctors at the stop. The basic Bouwers-Maksutov meniscus corrector principle has been utilized in a multitude of forms. A few of the possible Cassegrain embodiments of the principle are shown in Fig. 13.46. The reader can probably devise an equal number in a few minutes. An arrangement similar to that shown in Fig. 13.46c is frequently used in homing missile guidance systems. The corrector makes a reasonably aerodynamic window, or dome, and although the system is not concentric, the primary and secondary can be gimballed as a unit about the center of curvature of the dome so that the “axial” correction is maintained as the direction of sight is varied.

(a) An achromatized meniscus corrector. (b) An aspheric corrector plate at the stop removes the residual zonal spherical aberration of the concentric system.

Figure 13.45

The Design of Optical Systems: Particular

491

Figure 13.46 Four of the many possible Cassegrain versions of the

meniscus corrector catadioptric system..

There is a tremendous number of variations of the catadioptric principle. Refractive correctors in almost every conceivable form have been combined with mirrors. Positive field lenses have been used to flatten the overcorrected Petzval surface of the basic concave reflector, comacorrecting field elements have been used with paraboloids, and multiple nonmeniscus correctors have been used with spheres, to name just a few of the variations on the device. The basic strength of this general system is, of course, the relatively small aberration inherent in a spherical reflector; the corrector’s task is to remove the faults without losing the virtues. Two or more closely spaced thin-corrector elements whose total power is effectively zero can be shaped to correct the aberrations of a spherical mirror. If the glass is the same for all of the corrector elements, then the combination will have little or no chromatic, primary or secondary. Additional examples of catadioptric systems are shown in Figs. 14.29, 14.30, and 14.31. 13.6 The Rapid Estimation of Blur Sizes for Simple Optical Systems It is frequently useful to be able to estimate the size of the aberration blur produced by an optical system without going to the trouble of

492

Chapter Thirteen

making a raytrace analysis. In preliminary engineering work or the preparation of technical proposals, where time is limited, the following material (which is based largely on third-order aberration analysis or empirical studies) can be of value. The aberrations are expressed in terms of the angular size  (in radians) of the blur spot which they produce;  may be converted to B, the linear diameter of the blur, by multiplying by the system focal length. In this section the object will be assumed to be at infinity. Where the blur size for more than one aberration is given, the sum of all the aberration blurs will yield a conservative (i.e., large) estimate of the total blur. Where the blur is due to chromatic aberration, the blur angle given encompasses the total energy in the image of a point. Occasionally it is of value to know that 75 to 90 percent of the energy is contained in a blur one-half as large, and 40 to 60 percent of the energy is contained in a blur one-quarter as large as that given by the equations. In the visible, the chromatic blur is usually reduced by a factor of about 40 by achromatizing the system. The blurs given for spherical aberration are the minimum-diameter blur sizes; these values are the most useful for work with detectors. For visual or photographic work, a “hard-core” focus, as discussed in Chap. 11, is preferable, and the blurs given here should be modified accordingly. Note that with the exception of Eqs. 13.26 and 13.27, all the blurs are based on geometrical considerations. It is, therefore, wise to evaluate Eq. 13.26 or 13.27 first to be certain that the geometrical blurs are not smaller than the diffraction pattern before basing further effort on the geometrical results. More complete discussions of the individual systems may be found in the preceding section. Diffraction-limited systems.

The diameter of the first dark ring of the

Airy pattern is given by 2.44    radians D 1.22 B  2.44 (f/#)   NA

(13.26) (13.27)

where is the wavelength, D is the clear aperture of the system, (f/#)  f/D is the relative aperture, and f is the focal length. The “effective” diameter of the blur (for modulation transfer purposes) is about onehalf the above.

The Design of Optical Systems: Particular

493

Spherical mirror

0.0078 Spherical aberration:    radians (f/#)3

(13.28)

Sagittal coma:

(lp  R) Up   2 radians 16R (f/#)

(13.29)

Astigmatism:

(lp  R)2Up2    radians 2R2 (f/#)

(13.30)

where lp is the mirror-to-stop distance, R is the mirror radius, (lp  R) is the center-to-stop distance, and Up is the half-field angle in radians. The focal plane of a spherical mirror is on a spherical surface concentric to the mirror when the stop is at the center of curvature. Paraboloidal mirror

Spherical aberration:   0

(13.31)

Sagittal coma:

Up   2 radians 16 (f/#)

(13.32)

Astigmatism:

(lp  f) Up2    radians 2f (f/#)

(13.33)

where the symbols have been defined above. Schmidt system

Spherical aberration:

0

(13.34)

Higher-order aberrations:

Up2   3 radians 48 (f/#)

(13.35)

Spherochromatic:

1   3 256V (f/#)

(13.35a)

Mangin mirror (Stop at the mirror):

Zonal spherical:

103   4 radians 4 (f/#)

(13.36)

Chromatic aberration:

1    ) radians 6V (f/#

(13.37)

494

Chapter Thirteen

Sagittal coma:

Up   2 radians 32 (f/#)

(13.38)

Astigmatism:

Up2    radians 2 (f/#)

(13.39)

Simple thin lens.

(Minimum spherical shape):

K Spherical aberration:   3 radians (f/#) K  0.0067

for n  1.5

 0.027

for n  2.0

 0.0129

for n  3.0

 0.0103

for n  3.5

 0.0087

for n  4.0

1 Chromatic aberration:    radians 2V (f/#)

(13.40)

(13.41)

Sagittal coma:

Up   2 radians 16 (n  2) (f/#)

Astigmatism:

Up2    radians (at compromise focus) 2 (f/#) (13.43)

(13.42)

where n is the index of refraction, V is the reciprocal relative dispersion, and the stop is at the lens. Concentric Bouwers. The expressions for monochromatic aberrations

are empirical and are derived from the performance graphs and tables given by Bouwers and by Lauroesch and Wing (see references). Rear concentric (solid line in Fig. 13.44). The maximum corrector thickness of this form must be limited to keep the image from falling inside the corrector. With the thickest possible corrector: Zonal spherical:

4  104  ≈  radians (f/#)5.5

(13.44)

General concentric

Zonal spherical:

104   ≈ t radians  0.06 (f/#)5 f

冢

冣

(13.45)

The Design of Optical Systems: Particular

495

tf n Chromatic aberration:  ≈  2n2R1R2 (f/#) radians

(13.46a)

n t or very approximately:  ≈ 0.6   radians 2 f n (f/#)

(13.46b)

Corrected concentric

Higher-order aberrations: 9.75 (Up  7.2Up3) 105  ≈  radians (f/#)6.5

(13.47)

where t is the corrector plate thickness, f is the system focal length, n is the dispersion of the corrector material, n is the index of the corrector, and R1 and R2 are the radii of the corrector. These expressions apply for corrector index values in the 1.5 to 1.6 range and for relative apertures to the order of f/1.0 or f/2.0. For speeds faster than f/1.0, the monochromatic blur angles are larger than above (e.g., about 20 percent larger at f/0.7). The use of a high-index corrector (n  2) will reduce the monochromatic blur somewhat at high speeds. The charts of Figs. 13.47 to 13.54 are designed to give a rapid, albeit incomplete, estimation of the performance of the systems discussed in this section. Figure 13.47 is used by locating the intersection of a wavelength line with the appropriate diagonal aperture line. The linear blur spot diameter B may be converted to the angular blur spot diameter  by locating the abscissa corresponding to the intersection of the B diameter ordinate with the appropriate diagonal focal-length line. Figures 13.48, 13.49, and 13.51 assume that the aperture stop is in contact with the lens or mirror. The blur size for the angle-dependent aberrations is found by locating the intersection of a horizontal field angle line with the diagonal f-number line. Figure 13.52 plots the spherical aberration blur as a function of element shape and index of refraction. This plot makes the effect of a change of index quite apparent. As the index is increased, the spherical aberration is reduced, and the shape of the element which yields the minimum amount of spherical becomes more and more meniscus. This illustrates why lens designers use high-index glasses to improve a lens design. Note that the minimum spherical for an index of 4.0 is the same as that of a mirror. Figure 13.53 shows the effect of splitting an element into two or more elements. For an index of 1.5, splitting a lens in two reduces the spherical by a factor of about 5; dividing the lens into three parts reduces it by a factor of about 20. If the lens is split into four parts, the third-order spherical can be reduced to zero. This effect is widely uti-

496

Chapter Thirteen

Figure 13.47 Blur spot size chart for diffraction-limited systems. Diameter is

that of the first dark ring of the Airy disk.

lized to improve the image quality of more complex lenses. See, for example, Figs. 12.9, 13.20, and 13.21. A very rough idea of the geometrical modulation transfer factor of the system can be obtained by using Fig. 13.54. The total angular blur spot for the system is determined (by summing the individual aberration blurs) and is then multiplied by the desired spatial frequency in cycles per radian. The modulation transfer factor may then be read directly from the figure. Note that this is very approximate and is not reliable when the total blur is of the same order of magnitude as the Airy disk (see the discussion in Chap. 11).

The Design of Optical Systems: Particular

Figure 13.48 Blur spot size charts for spherical reflector. Charts B

and C also apply to a paraboloidal reflector; Fig. 13.47 may be used for a paraboloid on axis.

Figure 13.49 Blur spot size charts for Mangin mirrors.

497

498

Chapter Thirteen

Figure 13.50 Blur spot size chart. Chart A: Schmidt systems.

Charts B, C, and D: Concentric Bouwers systems.

Figure 13.51 Blur spot size charts for a single refracting ele-

ment.

The Design of Optical Systems: Particular

499

Figure 13.52 The angular spherical aberration blur

 of a single-lens element as a function of shape for various values of the index of refraction.  is the element power; y is the semiaperture. The angular blur can be converted to longitudinal spherical by LA  2/y2. (Object at infinity.)

Bibliography Note: Titles preceded by an asterisk (*) are out of print. See also references for Chap. 12. Benford, J., and H. Rosenberger, “Microscope Objectives and Eyepieces,” in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978.

500

Chapter Thirteen

Figure 13.53 The spherical aberration of one, two, three, and four thin lens-

es, each bent for minimum spherical aberration, as a function of the index of refraction. The number of elements in the set is i. (Object at infinity.)

The modulation transfer characteristic of a system with an angular blur  (in radians) for a sinusoidal object with a spatial frequency of v cycles per radian. This is a plot of MTF  2J1 (v)/v and assumes that the image blur is a uniformly illuminated disk.

Figure 13.54

Benford, J., “Microscope Objectives,” in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965. Betensky, E., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (photographic lenses). Betensky, E., M. Kreitzer, and J. Moskovich, “Camera Lenses” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 16.

The Design of Optical Systems: Particular

501

*Bouwers, W., Achievement in Optics, New York, Elsevier, 1950. Cook, G., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965 (photographic objectives). *Dimitroff and J. Baker, Telescopes and Accessories, London, Blakiston, 1945. Fischer, R. (ed.), Proc. International Lens Design Conf., S.P.I.E., vol. 237, 1980. Goldberg, N., “Cameras,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 15. Inoue, S., and R. Oldenboug, “Microscopes,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 17. Johnson, R. B., “Lenses,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 1. Jones, L., “Reflective and Catadioptric Objectives,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 18. Kingslake, R., Optics in Photography, S.P.I.E. Press, Bellingham, Wash., 1992. Kingslake, R., A History of the Photographic Lens, San Diego, Academic, 1989. Korsch, D., Reflective Optics, New York, Academic Press, 1991. Laikin, M., Lens Design, New York, Marcel Dekker, 1991. Lauroesch, T., and C. Wing, J. Opt. Soc. Am., vol. 49, 1959, p. 410 (Bouwers systems). Maksutov, D., J. Opt. Soc. Am., vol. 34, 1944, p. 270. Patrick, F., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 5, New York, Academic, 1965 (military optical instruments). Riedl, M. J., Optical Design for Infrared Systems, S.P.I.E., vol. TT20, 1995. Rosin, J., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965 (eyepieces and magnifiers). Rutten, H., and M. van Venrooij, Telescopic Optics, Richmond, VA, Willmann-Bell, 1988. Schroeder, D., Astronomical Optics, San Diego, Academic, 1987. Shannon, R., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (aspherics). Smith, W. J., Modern Lens Design, New York, McGraw-Hill, 1992. Smith, W. J. (ed.), Lens Design, S.P.I.E., vol. CR41, 1992. Smith, W., in W. Driscoll (ed.), Handbook of Optics, New York, McGraw-Hill, 1978. Smith, W., in Wolfe and Zissis (eds.), The Infrared Handbook, Washington, Office of Naval Research, 1985. Taylor, W., and D. Moore (eds.), Proc. International Lens Design Conf., S.P.I.E., vol. 554, 1985.

502

Chapter Thirteen

Exercises See the note preceding the exercises for Chapter 12. 1 Design a symmetrical eyepiece, using BK7 and SF2 glass, for a 10  telescope. 2 Design a separable (Lister) 10, NA 0.25 microscope objective by determining the zero spherical form for each doublet. Analyze the field curvature of the combination. 3 Design a 20 (f  8 mm) two-mirror reflecting microscope objective and determine an appropriate combination of aperture and field over which the aberrations will not exceed the Rayleigh limit. 4 Design a split-front crown triplet (see Fig. 13.21), using SK4 and SF5 glasses, for a speed of f/2.8, a focal length of 125 mm, and a total field of 20°, suitable for a 35-mm slide projector. 5 For an aperture of f/2 and a half-field of 0.1 radians, determine the relative angular-blur-spot size of the various systems listed in Section 13.6. Where stop position is critical, consider (a) the best position, and (b) the most compact arrangement. Assume a V of 100 for the refracting materials. 6 Design an f/1 Bouwers concentric system. Achromatize the design (choose a crown and flint with matching indices) and analyze the off-axis chromatic and chromatic variation of the aberrations.

Chapter

14 Some Forty-Four More Lens Designs

14.1 Introduction This chapter consists entirely of the design and performance data for forty-four additional lenses. These designs were selected from the nearly 300 lenses detailed in W. J. Smith, Modern Lens Design (MLD) (New York, McGraw-Hill, 1992). The figures are taken directly from MLD without change. Figures 14.1 and 14.2 are sample figures which are annotated to indicate the meaning of certain abbreviations used in the figures and also to show the scale of the aberration plots, respectively. All the designs are shown at a focal length of 100, regardless of the focal length at which they are actually apt to be used. The caption associated with each figure is rather limited. Should a more extensive

Figure 14.1 Sample lens prescription showing the abbrevia-

tion meanings.

503

504

Chapter Fourteen

Figure 14.2 Sample aberration plot showing the scale of each plot.

discussion of lens design theory, principles, and techniques be desired, the reader is referred to MLD itself. 14.2

The Designs

The designs and performance data are shown in Figs. 14.3 to 14.46. Bibliography Betensky, E., M. Kreitzer, and J. Moskovich, “Camera Lenses,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 16. Smith, W. J., Modern Lens Design, New York, McGraw-Hill, 1992.

Figure 14.3 This is an apochromatic triplet, corrected for spherical, chromatic, and

coma. Note that the spherochromatic is not corrected. (One definition of “apochromat” is that the chromatic is corrected for three wavelengths and the spherical aberration is corrected for two wavelengths.)

505

Figure 14.4 An airspaced triplet telescope objective. Splitting the crown element

powerfully reduces the zonal spherical, and spacing the flint away from the crowns works on both the zonal and the spherochromatism, leaving the secondary spectrum as the dominant axial aberration.

506

Some Forty-Four Lens Designs

507

Figure 14.5 A doublet magnifier. This is an excellent design for a general-purpose

magnifier or for a slide-viewer lens.

508

Chapter Fourteen

Figure 14.6 A simple, inexpensive eyepiece with a long eye relief and good performance,

often used as a microscope eyepiece.

Some Forty-Four Lens Designs

509

Figure 14.7 An example of the symmetrical, or Ploessl, eyepiece using dense barium

crown glass. This excellent general-purpose eyepiece is a very forgiving design in that almost any two achromats oriented crown to crown make a pretty good eyepiece or magnifier.

510

Chapter Fourteen

Figure 14.8 A classic Erfle eyepiece, used when one needs to cover a moderately

wide angle. The large eye relief and the flat Petzval field of the Erfle derive from the concave surface close to the focal plane.

Some Forty-Four Lens Designs

511

Figure 14.9 An unusual Cooke triplet with high-index crowns. The designer has used

thick elements to improve this design, which perhaps should disqualify it from the label “Cooke.”

512

Chapter Fourteen

Figure 14.10 A low-index, broadband Cooke triplet which uses calcium fluoride and fused

silica to allow coverage of a spectral band extending from the ultraviolet (UV) to the near infrared (IR). Note the large spherochromatism and reversed secondary spectrum.

Some Forty-Four Lens Designs

513

Figure 14.11 A relatively simple reversed telephoto, or retrofocus, which covers a wide

(±37°) field at f/2.8 and has a back focus over 30 percent longer than its focal length.

Figure 14.12 A “fish-eye” lens covers a 180° or larger field of view by taking advan-

tage of the heavy overcorrected spherical aberration of the powerful negative meniscus front elements, which strongly deviate the principal ray. This spherical aberration of the pupil causes the entrance pupil to move forward and off the axis and to tilt at wide angles of view.

514

Some Forty-Four Lens Designs

Figure 14.13 A typical telephoto lens with an 80 percent telephoto ratio; this config-

uration would make an excellent 35-mm camera lens at a 200-mm focal length.

515

Figure 14.14 The classic Dagor combines the front and rear doublets of the Protar

into a triplet. Note the progression of refractive index and the powers of the cemented surfaces. Later versions (see Fig. 13.13) split off the inner crowns, allowing the use of a higher-index glass for these elements. Note that the latter form has eight reflecting air glass surfaces vs. four for the Dagor, an important consideration in the days before low-reflection coatings. 516

Figure 14.15 The Dogmar is related to the Dagor and Protar in that it can be considered to

consist of two symmetrical meniscus triplet components, each with a central air lens. As shown here, the Dogmar makes an excellent enlarger lens, being relatively insensitive to conjugate change. 517

518

Chapter Fourteen

Figure 14.16 A Tessar with a reversed rear doublet. This orientation is said to be better

when a high-index rare earth crown is used in the doublet.

Some Forty-Four Lens Designs

Figure 14.17 An example of a reversed Tessar with the doublet in front.

519

520

Chapter Fourteen

Figure 14.18 The Heliar form has doublets front and rear, gaining the advantage of a

roughly symmetrical construction. Just as the Tessar is better than the Cooke triplet, the Heliar is better than the Tessar.

Some Forty-Four Lens Designs

521

Figure 14.19 An unclassified, good, but rarely encountered form, with a central negative

doublet replacing the flint of the Tessar. Note that the cemented surface of the inner doublet is a “Merté” surface, as also shown in Fig. 13.19.

522

Chapter Fourteen

Figure 14.20 A Petzval modification using dense barium crowns, with the split rear

doublet widely spaced so that its flint element acts as a field flattener.

Some Forty-Four Lens Designs

523

Figure 14.21 A modification of Fig. 14.20 which splits the positive elements to allow

both improved performance and a significant increase of the speed to f/1.4.

524

Chapter Fourteen

Figure 14.22 A split front crown in this Petzval lens allows a speed of f/1.25 using ordi-

nary glasses. But notice the extremely short back focal length (which facilitates the good performance by reducing the element powers compared with those required when a longer back focus is provided).

Some Forty-Four Lens Designs

525

The R-Biotar, an extremely high-speed lens of simple construction, designed as a radiographic camera lens, controls the higher-order aberrations by careful spacing and power distribution.

Figure 14.23

526

Chapter Fourteen

Figure 14.24 When the thickness is allowed to vary, the split-front triplet often takes

this form, where the first three elements look a bit like the front member of a doubleGauss design.

Some Forty-Four Lens Designs

527

Figure 14.25 A direct descendant from the split-front triplet design, this design replaces

elements two and three with a triplet component using a low-index glass instead of air to space elements two and three apart, plus a Tessar-type rear component.

528

Chapter Fourteen

Figure 14.26 A really high-speed Sonnar.

Some Forty-Four Lens Designs

529

Figure 14.27 The meniscus inner crown of the split-front triplet can advantageously be

made a doublet. This is about the simplest of the many modifications that this powerful basic design form has undergone.

530

Chapter Fourteen

Figure 14.28 An example of a high-power microscope objective in which the apla-

natic front hyperhemisphere is modified by introducing a concave front surface which, being near the focus, acts as a field flattener. Note also the use of calcium fluoride and FK51 glass to correct the secondary spectrum.

Some Forty-Four Lens Designs

Figure 14.29 Three singlet correctors, of the same glass, whose power totals zero,

are used to correct the aberrations of the spherical-surfaced Cassegrain configuration without introducing either primary or secondary chromatic aberration (but not without spherochromatism).

531

532

Chapter Fourteen

Figure 14.30 An aspheric meniscus corrector, a second surface primary mirror, the

meniscus corrector as the secondary mirror, and two field corrector lenses in the final convergent beam all combine in this multifeatured design with excellent color correction.

Some Forty-Four Lens Designs

533

Figure 14.31 A single-material catadioptric, corrected for primary and secondary col-

or, has Mangin mirrors for both primary and secondary reflectors.

534

Chapter Fourteen

Figure 14.32 This basic six-element double-Gauss uses high-index crowns to reach

a speed of f/1.25.

Some Forty-Four Lens Designs

535

Figure 14.33 This f/2.0 35-mm camera objective is the result (and best) of an extensive

design study reported by Mandler at the 1980 International Lens Design Conference.

536

Chapter Fourteen

Figure 14.34 The split rear crown double Gauss, probably the most effective of the basic

modifications to the double Gauss, allows a speed of f/1.4 in this 35-mm camera lens.

Some Forty-Four Lens Designs

537

Figure 14.35 Recent double-Gauss camera lenses have advantageously separated the

cemented front doublet of the split rear crown system. Many of the newer designs follow this configuration.

Figure 14.36 A very high-speed double Gauss at f/1.1, this split front and split rear crown

design can be improved by using BaSF6 (668-419) glass in the front element to correct the chromatic.

538

Figure 14.37 The strong negative outer meniscus elements in this wide-angle

design have two obvious functions. In what might be regarded as a sort of insideout Cooke triplet, the negative elements (in a relatively low axial ray height location) flatten the Petzval field. They also serve to lower the slope of the principal ray at the central positive components, thus reducing the angular field that these components must cover. 539

540

Chapter Fourteen

Figure 14.38 The increased complexity provided by two more elements than Fig.

14.37 allows a total field of 90° for this lens.

Some Forty-Four Lens Designs

541

Figure 14.39 This triplet with an aspheric field corrector is typical of the wide-angle,

short, point-and-shoot camera lenses made possible by the new fabrication techniques for aspherics.

Figure 14.40 This projection TV objective has four elements, each with one aspher-

ic surface. This is one of the benefits of injection-molded plastic elements. Note that many projection TV objective designs incorporate one high-powered glass element in order to achieve thermal focus stability (which is a real problem with plastic optics).

542

Some Forty-Four Lens Designs

Figure 14.41 One might regard this as an IR Cooke triplet. The odd (i.e., not typ-

ical of a Cooke triplet) element shapes are the result of the high refractive indices of the materials used in the IR region.

543

544

Chapter Fourteen

Figure 14.42 This four-element all-germanium IR design achieves a remarkable

speed of f/0.55. A design this fast is difficult to get started because the strongly sloping rays tend to miss surfaces or to encounter total internal reflection (TIR). This makes it difficult to find a starting design where all the rays can be traced through.

Some Forty-Four Lens Designs

Figure 14.43 This is an IR telescope of the type often used as a “front” for a scanning

system. The “eyepiece,” consisting of two facing meniscus elements, is quite typical of the breed.

545

Figure 14.44 This F-theta laser scanning lens is an obvious configuration for the task.

It has an external pupil at the scanning mirror and produces the right amount of distortion to achieve the required h  F  relationship between input beam angle and the image distance from the axis. Since the system is monochromatic, we can use a low-index crown for the negative elements and a high-index flint for the positive elements. This improves the Petzval field. The lens is, of course, a hyperchromat. 546

Figure 14.45 The ability to mold precision aspheric surfaces in either glass or plas-

tic has been widely used in singlet lenses for laser disk objectives. Note that the relatively large thickness and the second aspheric surface allow reduction of the undercorrected astigmatism which is always found in thin positive systems.

547

Figure 14.46 This is basically a doublet telescope objective for a monochromatic (laser)

system in which a single high-index glass is used and the spherochromatic is well corrected by the airspace, as explained in Chap. 12. The result is a lens which is well corrected for a wide range of (monochromatic) wavelengths and is thus usable with many different laser wavelengths. (Note that because it is not achromatic, it must be refocused when the wavelength is changed.) 548

Chapter

15 Optics in Practice

This chapter will briefly survey the factors involved in reducing an optical system to practice. A short description of the optical manufacturing process will be followed by a discussion of the specification and tolerancing of optics for the shop. The mounting of optical elements will be considered next, and the chapter will be concluded with a section on optical laboratory measurement techniques. 15.1 Optical Manufacture The starting point for quantity production of optics is most frequently a rough molded glass blank or pressing. This is made by heating a weighed chunk of glass to a plastic state and pressing it to the desired shape in a metal mold. The blank is made larger than the finished element to allow for the material which will be removed in processing; the amount removed must (at a minimum) be sufficient to clean up the outer layers of the blank which are of low quality and may contain flaws or the powdery fireclay used in molding. Typically a lens blank will be about 3-mm thicker than the finished lens and 2-mm larger in diameter. A prism blank will be large enough to allow removal of about 2 mm on each surface. These allowances vary with the size of the piece and are less for a clean blank. When the blank is of an expensive material, such as silicon or one of the more exotic glasses, the blanking allowances are held to the absolute minimum to conserve material. Although most blanks are single, a cluster form is frequently economical for small elements. A cluster may consist of five or ten blanks connected by a thin web which is ground off to free the individual Materials.

549

550

Chapter Fifteen

blanks. If molded blanks are unobtainable, either because of the small quantity involved or the type of material, a rough blank may be prepared by chipping or sawing a suitable shape from stock material. Rough blanks can be checked fairly satisfactorily for the presence of strain (which results from poor annealing of the glass) by the use of a polariscope. An accurate check of the index requires that a plano surface be polished on a sample piece; however, if a batch of blanks is known to have been made from a single melt or run of glass, only one or two of the blanks need be checked, because the index within a melt is quite consistent. Since the final annealing process raises the index, the presence of strain is frequently accompanied by a low index value. When the shape of a blank is such that there are large variations in thickness from center to edge, it is difficult to get a uniform anneal. A variation of index within the blank may result. This is especially true for certain of the exotic optical glasses which are difficult to anneal. Glass in slab form is easier to anneal uniformly and is thus more homogeneous; it is often required for especially critical lenses for this reason. The preliminary shaping of an element is often accomplished by using diamond-charged grinding wheels. In the case of spherical surfaces, the process involved is generating. The blank is rotated in a vacuum chuck and is ground by a rotating annular diamond wheel whose axis is at an angle to the chuck axis, as indicated in Fig. 15.1. The geometry of this arrangement is such that a sphere is generated; the radius is determined by the angle between the two axes and by the effective diameter of the diamond tool (which will usually overhang the edge of the lens). The thickness is, of course, governed by how far the work is advanced into the tool. Flat work can be roughed Rough shaping.

Figure 15.1 Schematic diagram of the generating

process. The annular diamond tool and the glass blank are both rotated. Since their axes intersect at an angle (), the surface of the blank is generated to a sphere of radius R  D/2 sin .

Optics in Practice

551

out in a similar manner, with the two axes parallel. Rectangular shapes can be formed by milling, again using diamond tools. It is customary to process optical elements in multiples by fastening or blocking a suitable number on a common support. There are two primary reasons for this: The obvious reason is economy, in that several elements are processed simultaneously; the less apparent reason is that a better surface results when the processing is averaged over the larger area represented by a number of pieces. The elements are fastened to the blocking tool with pitch, although various compounds of waxes and rosins are also used for special purposes. Pitch has the useful property of adhering tenaciously to almost anything which is hot and not sticking to cold surfaces. The pitch bond is readily broken by chilling the pitch to a brittle state and shocking it with a brisk but light tap. Typically the elements are fastened to the blocker by pitch buttons which are molded to the back of the elements (suitably warmed); the buttons are then stuck to the heated blocker, as indicated in Fig. 15.2. (The surfaces of the elements are maintained in alignment by placing the buttoned elements into a lay-in tool of the proper radius and then pressing the heated blocker into contact with the pitch buttons.) The cost of processing an element is obviously closely related to the number of elements which can be blocked on a tool. There is no simple way to determine this number exactly; however, the following expressions (which are “limiting-case” expressions, modified to fit the actual values) are accurate to within about one element per tool. Blocking.

Figure 15.2 Section of a blocking tool with blanks

fastened in place with buttons of blocking pitch. The maximum number of lenses that can be blocked on a tool is determined by the angle B (see Eq. 15.2).

552

Chapter Fifteen

For plano surfaces: 3 No. per tool   4

1

冢 冣  2 D t d

2

(15.1)

rounded downward to the nearest integer, where Dt is the diameter of the blocking tool and d is the effective diameter of the piece (and should include an allowance for clearance between the elements). For spherical surfaces: 6R2 No. per tool   d2

SH

1

  冤 R 冥 2

(15.2a)

where R is the surface radius, d is the lens diameter (including a clearance allowance), and SH is the sagittal height of the tool. For a tool which subtends 180°, SH  R and this reduces to 6R2 1.5 1 1 No. per tool      2   d2 2 (sin B) 2

(15.2b)

rounded downward to the nearest integer, where B is the half-angle subtended by the lens diameter (plus spacing allowance) from the center of curvature of the surface, as indicated in Fig. 15.2. Where there are only a few lenses per tool, the following tabulation for 180° tools is convenient and more accurate. No. per tool

Maximum d/Dt

Maximum sin B

2B

2 3 4 5 6 7 8 9 10 11 12

0.500 0.462 0.412 0.372 — 0.332 0.301 0.276 — 0.253 0.243

0.707 0.655 0.577 0.507 0.500 0.447 0.398 0.383 0.369 0.358 0.346

90° 81.79° 70.53° 60.89° 60° 53.13° 46.91° 45° 43.24° 41.88° 40.24°

The surface of the element is further refined by a series of grinding operations, performed with loose abrasive in a water slurry and cast iron grinding tools. If the elements have not been generated, the grinding process begins with a coarse, fast-cutting emery. Otherwise, it begins with a medium grade and proceeds to a very fine grade which imparts a smooth velvety surface to the glass. The grinding (and polishing) of a spherical surface is accomplished to a high degree of precision with relatively crude equipment by taking advantage of a unique property of a spherical surface, namely, that Grinding.

Optics in Practice

553

a concave sphere and a convex sphere of the same radius will contact each other intimately regardless of their relative orientations. Thus, if two mating surfaces which are approximately spherical are contacted (with abrasive between them) and randomly moved with respect to each other, the general tendency is for both surfaces to wear away at their high spots and to approach a true spherical surface as they wear. (For a detailed analytical treatment of the subject of relative wear in optical processing, the reader is strongly urged to consult the reference by Deve, listed at the end of this chapter.) Usually the convex piece (either blocker or grinding tool) is mounted in a power-driven spindle and the concave piece is placed on top as shown in Fig. 15.3. The upper tool is constrained only by a ball pinand-socket arrangement and is free to rotate as driven by its sliding contact with the lower piece; it tends to assume the same angular rate of rotation as the lower piece. The pin is oscillated back and forth so that the relationship between the two tools is continuously varied. By adjusting the offset and amplitude of the motion of the pin, the optician can modify the pattern of wear on the glass and thus effect minute corrections to the value and uniformity of the radius generated by the process.

Figure 15.3 In grinding (or polishing), a semirandom scrubbing action

is set up by the rotation of the lower (convex) tool about its axis and the back-and-forth oscillation of the upper (concave) tool. Note that the upper tool is free to rotate about the ball end of the driving pin and takes on a rotation induced by the lower tool.

554

Chapter Fifteen

Each successively finer grade of emery is used until the grinding pits left by the preceding operation are ground out. The mechanics of the polishing process are quite analogous to the grinding process. However, the polishing tool is lined with a layer of pitch and the polishing compound is a slurry of water and rouge (iron oxide) or cerium oxide. The polishing pitch will cold flow and thus take on the shape of the work in a very short time. The polishing process is a peculiar one that is still incompletely understood. It appears that the surface of the glass is hydrolyzed by the polishing slurry and the resulting gel layer is scraped away by the particles of polishing compound embedded in the polishing pitch. This analysis explains many of the phenomena associated with polishing, such as scratches and cracks which are “flowed” shut by polishing, but which later open up when heated or exposed to the atmosphere. But when one considers that historically, polishing tools have been made from materials as diverse as felt, lead, taffeta, leather, wood, copper, and cork, and that polishing compounds other than rouge have been successfully used, and that many optical materials (e.g., silicon, germanium, aluminum, nickel, and crystals) have a different chemistry than glass, it would seem that a variety of polishing mechanisms is quite likely. Some polishing agents are actually etchants of the material that they polish; some materials can be polished dry. Polishing is continued until the surface is free of any grinding pits or scratches. The accuracy of the radius is checked by the use of a test plate (or test glass). This is a very precisely made master gage which has been polished to an exact radius and which is a true sphere to within a tiny fraction of a wavelength. The test plate is placed in contact with the work, and the difference in shape is determined by the appearance of the interference fringes (Newton’s rings) formed between the two. The relative curvatures of the two surfaces can be determined by noting whether the gage contacts the work at the edge or the center. If the number of rings is counted, the difference between the two radii can be closely approximated from the formula Polishing.

2R

R ≈ N  d

冢 冣

2

(15.3)

where R is the radius difference, N is the number of fringes, is the wavelength of the illumination, R is the radius of the test plate, and d is the diameter over which the measurement is made. One fringe indicates a change of one-half wavelength in the spacing between the two surfaces. A noncircular fringe pattern is an indication of an aspheric surface. An elliptical fringe indicates a toroidal surface.

Optics in Practice

555

Small corrections are made either by adjustment of the stroke of the polishing machine or by scraping away portions of the polishing tool so that the wear is concentrated on the portion of the work which is too high. After both surfaces of an element are polished, the lens is centered. This is done by grinding the rim of the lens so that the mechanical axis (defined by the ground edge of the lens) coincides with the optical axis, which is the line between the centers of curvature of the two surfaces. In visual centering the element is fastened (with wax or pitch) to an accurately trued tubular tool on a rotating spindle. When the lens is pressed on the tool, the surface against the tool is automatically aligned with the tool and hence with the axis of rotation. While the pitch is still soft, the operator slides the lens laterally until the outer surface also runs true. If the lens is rotated slowly, any decentration of either surface is detectable as a movement of the reflected image (of a nearby target) formed by that surface, as indicated in Fig. 15.4. For high-precision work, the images may be viewed with a telescope or microscope to increase the operator’s sensitivity to the image motion. The periphery of the lens is then ground to the desired diameter with a diamond-charged wheel. Bevels or protective chamfers are usually ground at this time. For economical production of moderately precise optics, a mechanical centering process is used. In this method, called “cup” or “bell” centering, the lens element is gripped between two accurately trued tubular tools. The pressure of the tools causes the lens to slip sideways until the distance between the tools is at a minimum, thus centering the lens. The lens is then rotated against a diamond wheel to grind the diameter to size. Centering.

Figure 15.4 Left: In visual centering the lens is shifted laterally until no

motion of the image of a target reflected from the lens surface can be detected as the lens is rotated. Right: In mechanical centering the lens is pressed between hollow cylinders. It slides laterally until its axis coincides with the common axis of the two tools.

556

Chapter Fifteen

The manufacture of the lens is completed by low-reflection coating the surfaces as required and by cementing, if the element is part of a compound component; these processes are outlined in Chap. 7. Modifications of the standard processing techniques are sometimes required for unusual materials. Brittle materials (e.g., calcium fluoride) must be treated gently, especially in grinding. A finer, softer abrasive is required; sometimes soap is added to the abrasive and soft brass grinding tools are used in place of cast iron. At the other extreme, sapphire (Al2O3) cannot be processed with ordinary materials because of its extreme hardness, and diamond powder is used for both grinding and polishing. Materials which are subject to attack by the grinding or polishing slurry are sometimes processed using a saturated solution of the optical material in the liquid of the slurry. For example, if a glass is attacked by water, one could make up the slurry with water in which a powder of the glass has been boiled or soaked for several days. Alternately a slurry of kerosene or oil sometimes works well. Other liquids which have been used in slurries include ethylene glycol, glycerol, and triacetate. High-speed processing. For optics where the surface accuracy require-

ments are not high, the processes described above can be materially accelerated. Ordinary grinding usually takes tens of minutes. Polishing may take from 1 or 2 hours up to 8 or 10 hours in difficult cases. These operations can be speeded up by increasing both the speed of the spindle rotation and the pressure between work and tool. Tool wear and deformation are then a problem, so tools which are very resistant to change are used. Grinding is accomplished using tools faced with pellets or pads of diamond particles sintered in a metal matrix; loose abrasive is not used. This is called pellet grinding or pelgrinding. Polishing is done with a metal (typically aluminum) tool faced with a thin (0.01 to 0.02 in) layer of plastic (e.g., polyurethane). Processing times are to the order of minutes; a surface may be generated, ground, and polished in 5 or 10 minutes. Since the tools are not compliant, it is necessary that the radius from the generator have an exact relationship to the radius of the diamond pellet grinding tool, and that the ground radius match (to within a few fringes, à la Eq. 15.3) the radius required by the hard plastic polishing tool. This process is widely used for sunglasses, filters, inexpensive camera lenses, and the like. The surface geometry tends to be marginal as regards accuracy of figure, and the fixed-abrasive grinding does cause some subsurface fracturing, but the process is fast and economical. The tooling required and the fine-tuning adjustments of the steps of the process limit its application to large-quantity production.

Optics in Practice

557

Nonspherical surfaces. Aspherics, cylinders, and toroids do not share

the universality of the spherical surface, and their manufacture is difficult. While a sphere is readily generated by a random grinding and polishing (because any line through the center is an axis), optical aspherics have only one axis of symmetry. Thus the simple principle of random scrubbing which generates a sphere must be replaced by other means. An ordinary spherical optical surface is a true sphere to within a few millionths of an inch. For aspherics this precision can only be obtained by a combination of exacting measurement and skilled “hand correction” or its equivalent. Cylindrical surfaces of moderate radius can be generated by working the piece between centers (i.e., on a lathe). However, any irregularity in the process tends to produce grooves or rings in the surface. This can be counteracted by increasing the rate of working along the axis relative to the rate of rotation about the axis. It is difficult to avoid a small amount of taper (i.e., a conical surface) in working cylinders. Large-radius cylinders are difficult to swing between centers and are usually handled with an x-y rocking mechanism which constrains the axes of work and tool to parallelism so as to avoid a saddle surface. Aspherics of rotation, such as paraboloids, ellipsoids, and the like, can be made in modest production quantities if the precision required of the surface is of a relatively low order, as, for example, in an eyepiece. The usual technique is to use a cam-guided grinding rig (with a diamond wheel) to generate the surface as precisely as possible. The problem is then to fine-grind and polish the surface without destroying its basic shape. The difficulty is that any random motion which works the surface uniformly tends to change the surface contour toward a spherical form. Extremely flexible tools which can follow the surface contour are required; however, their very flexibility tends to defeat their purpose, which is to smooth or average out small local irregularities left in the surface by the generating process. Pneumatic (i.e., air-filled, elastic) or spongy tools have proved quite successful for this purpose. Where precise aspherics are required, “hand” or “differential” correction is practically a necessity. The surface is ground and polished as accurately as possible and is then measured. The measurement technique must be precise enough to detect and quantify the errors. For high-quality work, this means that the measurements must be able to indicate surface distortions of a fraction of a wavelength. The Foucault knife edge test and the Ronchi grating tests are widely used for this purpose; these tests can usually be applied directly to the aspheric surface, although there are many aspheric applications (e.g., the Schmidt corrector plate) where the test must be applied to the complete system to determine the errors in the aspheric.

558

Chapter Fifteen

When the surface is close to the required figure, it can be tested with an interferometer, just as a spherical surface on a lens is tested with a test plate (which is of course a simple interferometer). However, for a nonspherical surface some sort of arrangement is necessary to reshape the wave front reflected from the aspheric so that it matches the reference wave front of the interferometer. For a conic surface, auxiliary mirrors can be arranged so that the conic is imaging from focal point to focal point, and a perfect conic will then produce a perfectly spherical wave front. A more generally applicable approach is the use of a null lens, which is designed and very carefully constructed to distort the reflected wave front into an exactly spherical shape. For a paraboloid tested at its center of curvature, the null lens can be as simple as one or two plano-convex lenses whose undercorrected spherical cancels the overcorrection of the paraboloid. For general aspherics, the null lens may need to be quite complex. When the surface errors have been measured and located, the surface is corrected by polishing away the areas which are too high. This can be accomplished (with a full-size polisher and a very short stroke) by scraping away those areas of the polisher which correspond to the low areas of the surface. In making a paraboloid of low aperture, such as used in a small astronomical telescope, the surface is close enough to a sphere that the correction can often be effected simply by modifying the stroke of the polisher. However, for large work and for difficult aspherics, it is usually better to use small or ring (annular) tools and to wear down the high zones by a direct attack. A certain amount of delicacy and finesse is required for this approach; if the process is continued for a minute or so longer than required, the result is a depressed ring which then requires that the entire balance of the surface be worn down to match this new low point. A few companies have developed equipment which more or less automates this process. In one technique, a computer-controlled polisher uses a small polishing tool (or a tool consisting of three small tools which are driven to spin about their centroid) which is directed to dwell on the regions of the work which are high and need to be polished down. The location and dwell time are determined from interferograms of the surface, plus a knowledge of the wear pattern which the polishing tool produces. The use of a small, driven polisher means that the device is not limited to polishing annular zones on the work, and thus unsymmetrical surface errors can be efficiently corrected. Another computer-controlled process is called magnetorheologic polishing. Here the polishing slurry includes a magnetic iron compound. The slurry is moved past the rotating lens, and at the lens a magnetic field causes the slurry to become stiff. This produces a localized polishing (or wearing) action on the surface. By rocking, spinning, and

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559

advancing the lens into the moving slurry under computer control, the surface can be locally polished to achieve the desired surface figure. Again, an unsymmetrical figure error can be corrected by synchronizing the localized polishing action with the position of the lens. Extremely accurate, numerically controlled lathes and milling machines are now available which are capable of generating both the finish and the precise geometry required for an optical surface. The cutting tool used is a single-crystal diamond, and the optic is machined as in a lathe or as with a fly-cutter in a mill. A single-point machining operation leaves tool marks—the finished surface is scalloped, and in some respects resembles a diffraction grating. This is one limitation of the process, and finished surfaces are often lightly “postpolished” to smooth out the turning marks. The more severe limitation is that only a few materials are suitable for machining, and unfortunately, optical glass is not one of them. However, several useful materials are turnable, including copper, nickel, aluminum, silicon, germanium, zinc selenide and sulfide, and, of course, plastics. Thus mirrors and infrared optics can be fabricated this way. Infrared optics do not require the same level of precision as do visual-wavelength optics, simply because a quarter-wave is almost 20 times larger at 10 m than in the visible wavelengths. With this process an aspheric surface is just about as easy to make as a spherical surface. It has found significant acceptance in the infrared and military applications. Single-point diamond turning.

15.2

Optical Specifications and Tolerances

Many otherwise fully competent optical workers come to grief when it is necessary for them to send their designs to the shop for fabrication. The two most common difficulties are underspecification, in the sense of incompletely describing what is required, and overspecification, wherein tolerances are established which are much more severe than necessary. Optical manufacture is an unusual process. If enough time and money are available, almost any degree of precision (that can be measured) can be attained. Thus, specifications must be determined on a dual basis: (1) the limits which are determined by the performance requirements of the system, and (2) the expenditure of time and money which is justified by the application. Note well that optical tolerances which represent an equal amount of difficulty to maintain may vary widely in magnitude. For example, it is not difficult to control the sphericity of a surface to one-tenth of a micrometer; the comparable (in terms of difficulty) tolerance for thickness is about 100 m (0.1 mm),

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three orders of magnitude larger. For this reason it is rare to find “box” tolerances in optical work; each dimension, or at least each class of dimension, is individually toleranced. Every essential characteristic of an optical part should be spelled out in a clear and unambiguous way. Optical shops are accustomed to this, and if a specification is incomplete, either time must be wasted in questioning the specification to determine what the requirements are, or the shop must arbitrarily establish a tolerance. Either procedure is undesirable. The following paragraphs are an attempt to provide a general guide to the specification of optics. The discussion will include the basis for the establishment of tolerances, the conventional methods of specifying desired characteristics, and an indication of what tolerances a typical shop may be expected to deliver. The intelligent choice of specifications and tolerances for optical fabrications is an extremely profitable endeavor. The guiding philosophy in establishing tolerances should be to allow as large a tolerance as the requirement for satisfactory performance of the optical system will permit. Designs should be established with the aim of minimizing the effect produced by production variations of dimensions. Frequently, simple changes in mounting arrangements can be made which will materially reduce fabrication costs without detriment to the performance of a system. One should also be certain that the tightly specified dimensions of a system are the truly critical dimensions, so that time and money are not wasted in adhering to meaningless demands for accuracy. Surface quality. The two major characteristics of an optical surface are

its quality and its accuracy. Accuracy refers to the dimensional characteristics of a surface, i.e., the value and uniformity of the radius. Quality refers to the finish of the surface, and includes such defects as pits, scratches, incomplete or “gray” polish, stains, and the like. Quality is usually extended to similar defects within the element, such as bubbles or inclusions. In general (with the exception of incomplete polish which is almost never acceptable) these factors are merely cosmetic or “beauty defects” and may be treated as such. The percentage of light absorbed or scattered by such defects is usually a completely negligible fraction of the total radiation passing through the system. However, if the surface is in or near a focal plane, then the size of the defect must be considered relative to the size of the detail it may obscure in the image. Also, if a system is especially sensitive to stray radiation, such defects may assume a functional importance. In any case, one may evaluate the effect of a defect by comparing its area with that of the system clear aperture at the surface in question.

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The standards of military specification MIL-O-13830 (now formally obsolete) are widely utilized in industry. The surface quality is specified by a number such as 80-50, in which the first two digits relate to the apparent width of a tolerable scratch and the second two indicate the diameter of a permissible dig, pit, or bubble in hundredths of a millimeter. Thus, a surface specification of 80-50 would permit a scratch of an apparent width which matched (by visual comparison) a #80 standard scratch and a pit of 0.5-mm diameter. The total length of all scratches and the number of pits are also limited by the specification. In practice, the size of a defect is judged by a visual comparison with a set of graded standard defects. Digs and pits can, of course, be readily measured with a microscope; unfortunately the apparent width of a scratch is not directly related to its physical size, and this portion of the specification is not as well founded as one might desire. The concept of a visual comparison with a standard is a good and efficient one. McLeod and Sherwood, who originated this method of specifying surface quality, in their article describing it said that the number of a scratch was equal to the measured width in microns (micrometers) of a scratch made by a certain technique. Recently the government has used a relationship which indicates that the width in micrometers is only one-tenth of the scratch number. There is a widespread (and not unreasonable) suspicion that the widths of the standard scratches (which are maintained on physical pieces of glass) have become smaller in the decades since the 1940s (when the system originated.) Surface qualities of 80-50 or coarser (i.e., larger) are relatively easily fabricated. Qualities of 60-40 and 40-30 command a small premium in cost. Surfaces with quality specifications of 40-20, 20-10, 10-5, or similar combinations require extremely careful processing, and the more critical are considerably more expensive to fabricate. Such specifications are usually reserved for field lenses, reticle blanks, or laser optics. Surface accuracy. Surface accuracy is usually specified in terms of the

wavelength of light from a sodium lamp (0.0005893 mm) or HeNe laser (0.0006328 mm). It is determined by an interferometric comparison of the surface with a test plate gage, by counting the number of (Newton’s) rings or “fringes” and examining the regularity of the rings. As previously mentioned, the space between the surface of the work and the test plate changes one-half wavelength for each fringe. The accuracy of the fit between work and gage is described in terms of the number of fringes seen when the gage is placed in contact with the work. Test plates are made truly flat or truly spherical to an accuracy of a small fraction of a fringe. Spherical test plates, however, have radii which are known to an accuracy only as good as the optical-mechanical means which are used to measure them. Thus the radius of a test

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plate is frequently known only to an accuracy of about one part in a thousand or one part in ten thousand. Further, test plates are expensive (several hundred dollars per set) and are available as “stock tooling” only in discrete steps. Thus it frequently pays to enquire what radii the optical shop has as standard tooling. The usual shop specification for surface accuracy is thus with respect to a specific test plate, and it takes the form of requiring that the piece must fit the gage within a certain number of rings and must be spherical (or flat in the case of plane surfaces) within a number of rings. A fit of from five to ten rings, with a sphericity (or “regularity”) of from one-half to one ring is not a difficult tolerance. Fits of from one to three rings with correspondingly better regularity can be achieved in large-scale production at a very modest increase in cost. Note that an irregularity of a small fraction of a ring is difficult to detect when the fit is poor. Thus, little is saved by specifying a ten-ring fit and a quarter-ring sphericity, since the fit must be considerably better than ten rings to be certain that the irregularity is less than one-quarter ring. The usual ratio is to have a fit of no worse than four or five times the maximum allowable irregularity. The change in radius due to a poor fit is frequently negligible in effect. For example, the radius difference between two (approximately) 50-mm radii at a 30-mm diameter which corresponds to five rings is (by Eq. 15.3) only about 33 m. The surface figure can be measured easily with an interferometer. While it is more difficult to control radius value with an interferometer than with a test plate, the interferometer is far superior when it comes to testing for sphericity or regularity. This is because the effective radius of the comparison wave front can be adjusted to match that of the surface under test, and also because the viewpoint of the interferometer is always normal to the surface and is thus not subject to the obliquity errors which afflict test plate readings. If possible, one should avoid specifying accurate surfaces on pieces whose thickness-to-diameter ratio is low. Such elements tend to spring and warp in processing, and extreme precautions are necessary to hold an accurate surface figure. A common rule of thumb is to make the axial thickness at least one-tenth of the diameter for negative elements; where there is a good edge thickness, one-twentieth or one-thirtieth of the diameter is sometimes acceptable. For extremely precise work, especially on plane surfaces, the optician might prefer a thickness of one-fifth to one-third of the diameter. The performance effects of errors in radius values (i.e., departures from the nominal design radii) are usually not too severe. In fact, it is the practice of some purchasers of optics not to indicate a tolerance on the specified radii, but to specify final performance in terms of focal length and resolution. It is usually possible for a well-tooled optical

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shop to select judiciously (from its tooling list) nearby radii which produce a result equivalent to the nominal design. If tolerances are specified on radius values, one should bear in mind the fact that most effects produced by a radius variation are not proportional to R, but to C (or R/R2). To take a simple example, we can differentiate the thin-lens focal-length equation 1 1 1     (n  1) (C1  C2)  (n  1)    f R1 R2

冢

冣

with respect to the first surface to get the following: d  (n  1) dC1 dR1 df  f 2 (n  1) dC1  f 2 (n  1)  R12 In a more complex system, the change in focal length resulting from a change in the ith curvature is approximated by

冢 冣

yi df ≈  f 2 (n′i  ni) dci y1

冢 冣

dRi yi df ≈  f 2 (n′i  ni)  y1 Ri2 The point is that if a uniform tolerance is to be established for all radii in a system, the uniform tolerance should be on curvature, not on radius. Therefore, radius tolerances should be proportional to the square of the radius. For example, given a lens with a radius of 1 in on one side and a radius of 10 in on the other, if we vary the 1-in radius by 0.001 in, the effect on the focal length is the same as a change of 0.100 in on the 10-in radius. If the second surface had a radius of 100 in, then the equivalent change would be about 10 in. The preceding is, of course, based on focal-length considerations only. With regard to aberrations, it is difficult to generalize, since one surface of a system may be very effective in changing a given aberration while another may be totally ineffective. The relative sensitivity is determined by the heights of the axial and principal rays at the surface, the index break across the surface, and the angles of incidence at the surface. A good estimate of the effect that any tolerance has on the aberrations of a system can be determined by use of the third-order surface contribution equations of Chap. 10. The effect of surface irregularity is more readily determined. Consider the case where the Newton’s rings are not circular; this is an indication of axial astigmatism, since the power in one meridian is stronger than in the other. Here it is convenient to call on the Rayleigh

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quarter-wave criterion. The OPD produced by a “bump” of height H on a surface is equal to H(n′  n), or, expressing it in terms of interference rings (remembering that each fringe represents one-half wavelength change in surface contour), OPD  1 2 (#FR) (n′  n) wavelengths where (#FR) is the number of fringes of irregularity. Thus, to stay within the Rayleigh criterion, the total OPD, summed over the whole system, should not exceed one-fourth wavelength; this is expressed by the following inequality: ∑ (#FR) (n′  n)  0.5 Thus, a single element of index 1.5 could have one-half fringe of astigmatism (or any other surface irregularity) on both surfaces before the Rayleigh criterion was exceeded (assuming that the nominal correction was perfect and that the irregularities were additive). Note that the expressions above do not take into account the fact that the system will probably be refocused to minimize the effects of any surface irregularity. See the discussion of OPD and spherical aberration in Sec. 11.3, for example. For astigmatism, refocusing reduces the OPD by a factor of 2. Thickness. The effects of thickness and spacing variation on the per-

formance of a system are readily analyzed, either by raytracing or by a third-order aberration analysis. The importance of thickness variation differs greatly from system to system. In the negative doublets of a Biotar (double-Gauss) objective, the thickness is extremely critical, especially as regards spherical aberration; for this reason the crown and flint elements are usually selected so that their combined thickness is very close to the design nominal. At the other extreme, the thickness variation of a planoconvex eyepiece element may be almost totally ignored, since it ordinarily has little or no effect on anything. In general, thicknesses and spacings may be expected to be critical where the slope of the marginal axial ray is large. Anastigmats in general, and meniscus anastigmats in particular, are prone to this sensitivity. High-speed lenses, large-NA microscope objectives, and the like are usually sensitive. Unfortunately the thickness of an optical element is not as readily controlled as some of the other characteristics. In production procedures where many elements are processed on the same block, the maintenance of a uniform nominal thickness requires precise blocking and tooling. The grinding operation, while precise enough in terms of radius, is difficult to control in terms of its extent. For close thickness

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control, the generating operation must be accurate and each subsequent grinding stage must be exactly timed so that the proper finish, radius, and thickness are arrived at simultaneously. A reasonable thickness tolerance for precise work is ±0.1 mm (±0.004 in). This can cause a shop some difficulty on certain lens shapes and on larger lenses; where a relaxation is possible, a tolerance of ±0.15 or ±0.2 mm is more economical. It is possible to hold ±0.05 mm in large-scale production by taking care throughout the fabrication procedure. The rejection rate at this tolerance can become disastrous if the smallest mischance occurs. Of course it is possible, by handworking and selection, to produce pieces to any desired tolerance level; the author has seen ±0.01 mm held in moderate production quantities (although at rather immoderate cost). The tolerances in centering are (1) on the diameter of the piece, and (2) on the accuracy of the centering of the optical axis with the mechanical axis. If the piece is to be centered (i.e., as a separate operation), the diameter can be held to a tolerance of plus nothing, minus 0.03 mm by ordinary techniques, and this is the standard tolerance in most shops. A small economy is effected by a more liberal tolerance. Tighter tolerances are possible, but are not often necessary for ordinary work. The concentricity of an element is most conveniently specified by its deviation. This is the angle by which an element deviates an axial ray of light directed toward the mechanical center of the lens. The deviation angle is an especially useful measure of decentration, since the deviation of a group of elements is simply the (vector) sum of the deviations of the individual elements. Figure 15.5 is an exaggerated sketch of a decentered element. The optical and mechanical axes are shown separated by an amount (the decentration). Since a ray parallel to the optical axis must pass through the focal point, the angular deviation  in radians of the ray aimed along the mechanical axis is given by the decentration divided by the focal length. Centering.

Figure 15.5 Showing the relationships between the optical

and mechanical axes, and the decentration and angle of deviation in a decentered lens.

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  (15.4) f Note that a decentered element may be regarded as a centered element plus a thin wedge of glass. The angle of the wedge W is given by the difference between the maximum and minimum edge thicknesses divided by the diameter of the element Emax  Emin W   radians (15.5) d Since the deviation of a thin prism is given by D  (n  1)A, we can similarly relate the wedge angle of an element to its deviation by   (n  1) W radians

(15.6)

If an element is centered on a high-production mechanical (clamping) centering machine, the limit on the accuracy of the concentricity obtained is determined by the residual difference in edge thickness which the cylindrical clamping tools cannot “squeeze out.” On most machines, this is to the order of 0.0005 in when residual tooling and spindle errors are also taken into account. Thus the residual wedge angle for a lens with a diameter d is given by 0.0005 in W   d and the resulting deviation is 0.0005 in (n  1)    d Thus, for ordinary lenses (n  1.5 to 1.6) a reasonable estimate of the deviation is given by 1    minutes (15.7) d where d is in inches, and the centering is done mechanically. If the centering is accomplished visually (as indicated in the left-hand sketch of Fig. 15.4) then the ability of the eye to detect motion is the limiting factor. If we assume that the eye can detect an angular motion of 6 or 7  105 radians, then the deviation will be approximately 1   (n  1)  ± 0.06 ± (contact and spindle errors) (15.8) R where  is in minutes and R is the radius of curvature of the outer surface in inches.*

冢

冣

*Equation 15.8 assumes that the image reflected from the outer radius is viewed at 10 in. This is obviously impossible if R is a convex surface with a radius longer than 20 in, and it is impractical if R is a long concave radius. Thus for |R|  20 in, one should substitute 0.05 for the 1/R term.

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The term (n  1)/R is from the visually undetected “wobble” of the outer radius and the 0.06 (n  1) term is due to the tilt in the tool which the eye could not detect in the truing of the tool (this is tested by pressing a flat glass plate against the rotating tool and observing any motion in the reflected image). The eye can, of course, be aided by means of a telescope or microscope which will further reduce the amount of decentration which can be detected by a factor equal to the magnification. Occasionally lenses are not put through a separate centering operation. When this is the case, the concentricity of the finished lens is determined by the wedge angle which is left in by the grinding operations. If the blocking tooling is carefully worked out, it is possible to produce elements with a wedge (i.e., the difference between the edge thickness of opposite edges) to the order of 0.1 or 0.2 mm. Centering is often omitted on inexpensive camera lenses, condensers, magnifiers, or almost any single element of a simple optical system. Simple elements made from rounded circles of window glass are often left uncentered. Prism dimensions and angles. The linear dimensions of prisms can be held to tolerances approximating those of an ordinary machined part, although the fabrication requirements of a prism are more difficult because of the finish and accuracy requirements of an optical surface. Thus tolerances of 0.1 or 0.2 mm are usually reasonable and tighter tolerances are possible. Prism angles can be held to within 5 or 10 minutes of nominal by the use of reasonably good blocking forms. Indeed it is possible, although exceedingly difficult, to make angles accurate to a few percent of these tolerances if one takes exquisite pains with the design, fabrication, correction, and use of the blocking tools. Usually angles which must be held to tolerances of a few seconds (such as roof angles) are “hand corrected.” Such angles are checked with an autocollimator, either by comparison with a standard or by using the internal reflections to make the piece a retrodirector. Angles of 90° and 45° among others can be self-checked in this way since their internal reflections form constant-deviation systems of 180° deviation (as discussed in Chap. 4). Prism size tolerances are usually based on the necessity to limit the image displacement errors (lateral or longitudinal) which they produce. Angular tolerances are usually established to control angular deviation errors. One can usually find one or two angles in a prism system which are more critical than the others; these can be tightly controlled and the other angles allowed to vary. For example, with respect to the deviation of a pentaprism, an angular error in the 45° angle between the reflecting faces is six times as critical as an error in the 90° angle between the entrance and exit faces, and the other two

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angles have no effect on the deviation. On occasion, prism tolerances are based on aberration effects. Since a prism is equivalent to a plane parallel plate and introduces overcorrected spherical and chromatic; an increase in prism thickness in a nominally corrected system will overcorrect these aberrations. Some prism angle errors are equivalent to the introduction of thin-wedge prisms into the system. The angular spectral dispersion of a thin wedge is (n  1)W/V (where W is the wedge angle and V is the Abbe V-value of the glass) and the resultant axial lateral color may limit the allowable angular tolerances. The characteristics of the refractive materials used in optical work which are of primary concern are index, dispersion, and transmission. For ordinary optical glass procured from a reputable source, visual transmission is rarely a problem. Occasionally, where a thick piece of dense glass is used in a critical application, transmission limits or color must be specified. Similarly, the dispersion, or V-value, is seldom a problem, except in special cases. For apochromatic systems where the partial dispersion ratio is exceedingly critical, very special precautions are required. The index of refraction is usually of prime concern in optical glass. As indicated in Chap. 7, the standard index tolerance is ±0.001 or ±0.0015, depending on the glass type. The glass supplier can hold the index more closely than this by selection or by extra care in the processing; either increases the cost somewhat. In practice the glass supplier will ordinarily use up only a fraction of this tolerance, since the index within a single melt or batch of glass is remarkably consistent. Thus, within a single lot of glass the index may vary only one in the fourth place. However, bear in mind that this variation may be centered about a value which is 0.001 or 0.0015 from the nominal index. It is sometimes economical to accept the standard tolerance and to adjust a design to compensate for the variation of a lot of glass in cases where the index is critical. Transmission and spectral characteristics are often poorly specified. For filters and coatings, ambiguity can usually be avoided by specifying spectral reflection (or transmission) graphically, i.e., by indicating the area of the reflection (or transmission) versus wavelength plot within which the characteristics of the part must lie. One should also indicate whether or not the spectral characteristics outside the specified region are of importance. For example, in a bandpass filter, it is important to indicate how far into the long- and short-wavelength regions the blocking action of the filter must extend. Figure 15.6 is a table of typical tolerances and may be used as a guide. Bear in mind, however, that the values given are typical and that there are many special cases that this sort of tabulation cannot cover. Materials.

569

Figure 15.6 Tabulation of typical optical fabrication tolerances.

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Additive tolerances. In analyzing an optical system to determine the

tolerances to be applied to specific dimensions, one can readily calculate the partials of the system characteristics with respect to the dimensions under consideration. Thus, one obtains the value of the partial derivative of the focal length (for example) with respect to each thickness, spacing, curvature, and index; likewise for the other characteristics, which may include back focus, magnification, field coverage, as well as the aberrations or wave-front deformations. Then each dimensional tolerance, multiplied by the appropriate derivative, indicates the contribution of that tolerance to the variation of the characteristic. Now if it were necessary to be absolutely certain that (for example) the focal length did not vary more than a certain amount, one would be forced to establish the parameter tolerances so that the sum of the absolute values of the derivative-tolerance products did not exceed the allowable variance. Although this “worst-case” approach is occasionally necessary, one can frequently allow much larger tolerances by taking advantage of the laws of probability and statistical combination. As a simple example, let us consider a stack of disks, each 0.1 in thick. We will assume that each disk is made to a tolerance of ±0.005 in and that the probability of the thickness of the disk being any given value between 0.095 and 0.105 in is the same as the probability of its being any other value in this range. This situation is represented by the rectangular frequency distribution curve of Fig. 15.7a. Thus, for example, there is 1 in 10 chance that any given disk will have a thickness between 0.095 and 0.096 in. Now if we stack two disks, we know that it is possible for their combined thicknesses to range from 0.190 to 0.210 in. However, the probability of the combination having either of these extreme thickness values is quite low. Since the probability of either of the disks having a thickness between 0.095 and 0.096 is 1 in 10, if we randomly select two disks, the probability of both falling in this range is 1 in 100. Thus, the probability of a pair of disks having a thickness between 0.190 and 0.192 is 1 in 100; similarly for a combined thickness of 0.208 to 0.210 in. The probability of a combined thickness of 0.190 to 0.191 (or 0.209 to 0.210) is much less; 1 in 400. The frequency distribution curve representing this situation is shown in Fig. 15.7b as a triangular distribution. Figure 15.7c shows frequency distribution curves for 1-, 2-, 4-, 8-, and 16-element assemblies. These curves have been normalized so that the area under each is the same and the extreme variations have been equalized. The important point here is that the probability of an assembly taking on an extreme value is tremendously reduced when the number of elements making up the assembly is increased. For example, in a stack of 16 disks with a nominal total thickness of 1.6 in and a possible

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Figure 15.7 Showing the man-

ner in which additive tolerances combine in assembly. Plot A shows a uniform probability in a dimension of a single piece. When two such pieces are combined, the resulting frequency distribution is shown in B. Normalized curves for assemblies of 1, 2, 4, 8, and 16 pieces are shown in C.

variation in thickness of ±0.080 in, the probability of a random stack having a thickness less than 1.568 in or more than 1.632 in (i.e., ±0.032 in) is less than 1 in 100. The importance of this in setting tolerances is immediately apparent. In the stacked-disks example, if the range of thicknesses represented by 1.568 to 1.632 in for 16 disks were the greatest variation that could be tolerated, we could be absolutely sure of meeting this requirement only by tolerancing each individual disk at ±0.002 in. However, if we were willing to accept a rejection rate of 1 percent in large-scale production, we could set the thickness tolerance at ±0.005 in. If the cost of the pieces made to the tighter tolerance exceeded the cost of the pieces made to the looser tolerance by as little as 1 percent (plus one sixteen-hundredth of the assembly, processing, and final inspection costs), the looser tolerance would result in a less costly product. In a frequency distribution curve such as those shown in Fig. 15.7 the area under the curve between two abscissa values represents the (relative) number of pieces which will fall between the two abscissa values. Thus the probability of a characteristic falling between two values is the area under the curve between the two abscissas divided by the total area under the curve.

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The “peaking-up” characteristic of multiple assemblies can also be represented by the two plots shown in Fig. 15.8. The graph on the left shows the percentage of assemblies which fall within a given central fraction of the total tolerance range as a function of that fraction. The number of elements per assembly is indicated on each curve. These curves were derived from Fig. 15.7c. The graph on the right in Fig. 15.8 is simply another way of presenting the same data. If one were interested in an assembly of 10 elements, the intersection of the abscissa corresponding to 10 and the appropriate curve would indicate that all but 0.2 percent (using the 99.8 percent curve) of the assemblies would fall within 0.55 of the total tolerance range represented by the sum of all 10 tolerances, and that over one-half of the assemblies (using the 50 percent curve) would fall within 0.15 of the total possible range. The preceding discussion has been based upon the unlikely assumptions that (1) each individual piece had a rectangular frequency distribution, and (2) each tolerance was equal in effect. This is rarely true in practice. The frequency distribution will, of course, depend on the techniques and controls used in fabricating the part, and the tolerance sizes may represent the partial derivative tolerance products from such diverse sources as tolerances on index, thickness, spacing, and curvature. Note, however, that in Fig. 15.7c the progression of curves may be started at any point. If, for example, the production methods produce a triangular distribution (such as that shown for an assembly of two elements), then the curve marked 4 (for “four elements”) will be the frequency distribution for two elements (of triangular distribution) and so on. Note also that as more and more elements are included in the assembly, the curve becomes a closer and closer approximation to the normal distribution curve which is so useful in statistical analysis

Figure 15.8 Probability distributions of additive tolerances in multiple assemblies.

See text for details.

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(except that the tolerance-type curves do not go to infinity as do normal curves). One useful property of the normal curve for an additive assembly is that its “peakedness” is proportional to the square root of the number of elements in assembly. Thus if 99 percent of the individual pieces are expected to fall within some given range, then for an assembly of 16 elements, 99 percent would be expected to fall within 兹苶 1/16, or one-quarter of the total range. A brief examination will indicate that even the rectangular distribution assumed for Figs. 15.7 and 15.8 tends to follow this rule when there are more than a few elements in the assembly. A rule of thumb frequently used to establish tolerances may be represented as follows:

冪莦 n

T≈

t 冱 i1

2 i

(15.9)

This is frequently referred to as the RSS rule, shorthand for the square root of the sum of the squares. What the RSS rule means is this: If some percentage (say 99 percent) of the part tolerances produces effects less than t (and varies according to a normal, or gaussian, distribution), then the same percentage (i.e., 99 percent in our example) of the assemblies will show a total tolerance effect less than T. While this section may seem to be a far cry from optical engineering, consider that a simple Cooke triplet has the following dimensions which affect its focal length and aberrations: six curvatures, three thicknesses, two spacings, three indices, and three V-values. These total fourteen for monochromatic characteristics and seventeen for chromatic aberrations. Such a system is eminently qualified for statistical treatment. Note that the validity of this approach does not depend on a large production quantity; it depends on a random combination of a certain number of tolerance effects. There are two obvious features of the RSS rule which are well worth noting. One is the square root effect: If you have n tolerance effects of a size ±x, then the RSS rule says that a random combination will produce an effect equal to ±x times the square root of n. For example, given 16 tolerance effects of ±1 mm, we should expect a variation of only ±4 mm, not ±16 mm. The other feature is that the larger effects dominate the combination. As an example, consider a case with nine tolerances of ±1 mm and one tolerance of ±10 mm. If we use the RSS rule on this, we get an expected variation equal to the square root of 109, or ±10.44 mm. Compare this with the fact that the single ±10-mm tolerance has an RSS of ±10 mm. The addition of the nine ±1-mm tolerances changed the expected variation by only 4.4 percent.

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One possible way to establish a tolerance budget using this principle is as follows: 1. Calculate the partial derivatives of the aberrations with respect to the fabrication tolerances (radius, asphericity, thickness and spacing, index, homogeneity, surface tilt, etc.). Express the aberrations as OPDs (wave-front deformation). 2. Select a preliminary tolerance budget. Figure 15.6 can be used as a guide to appropriate tolerance values. 3. Multiply the individual tolerances by the partial derivatives calculated in step 1. 4. Compute RSS for all the aberrations for each individual tolerance. This will indicate the relative sensitivity of each tolerance. 5. Compute RSS for all of the effects calculated in step 4 combined. 6. Compare the results of step 5 with the performance required of the system. This can be done by computing the RSS for the design OPD (as indicated by its MTF or whatever measure is convenient) combined with the tolerance budget OPD and using the material of Chap. 11 to determine the resulting MTF or Strehl ratio. 7. Adjust the tolerance budget so that the result of step 6 is equal to the required performance. Since the larger effects dominate the RSS, if you are tightening the tolerances (as is quite likely on the first go-round), you should tighten the most sensitive ones (and possibly loosen the least sensitive). Note that there is no economic gain if you loosen tolerances beyond the level at which costs or prices cease to go down. Conversely, one should be sure that the tolerances are not tightened beyond a level at which fabrication becomes impossible—since cost rises asymptotically toward infinity as this level is approached. 8. After one or two adjustments (steps 2 through 7) the tolerance budget should converge to one which is reasonable economically and which will produce an acceptable product. If the tolerances necessary to get an acceptable performance are too tight to be fabricated economically, there are several ways which are commonly used to ease the situation: 1. A test plate fit is a redesign of the system using the measured values of the radii of existing test plates. This eliminates the radius tolerance (except for the variations due to the test glass “fit” in the shop, and any error in the measurement of the radius.)

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2. A melt fit can effectively eliminate the effects of index and dispersion variation. Again, this is a redesign, using the measured index of the actual piece of glass to be used, instead of the catalog values. 3. A thickness fit uses the measured thicknesses of the actual fabricated elements to be assembled; this amounts to an adjustment of the airspaces during the assembly process. The redesigns called for in all three “fitting” operations above, while hardly trivial, are not major undertakings when an automatic lens design program is used. While the above may tend to induce a desirable relaxation in tolerances, one or two words of caution are in order. As previously mentioned, the index of refraction distribution within a melt or lot of glass may or may not be centered about the nominal value. When it is centered about a nonnominal value, the preceding analysis is valid only with respect to the central value, not the nominal value. Further, in some optical shops, there is a tendency to make lens elements to the high side of the thickness tolerance; this allows scratched surfaces to be reprocessed and will, of course, upset the theoretical probabilities. Another tendency is for polishers to try for a “hollow” test glass fit, i.e., one in which there is a convex air lens between the test plate and the work. This is done because a block of lenses which is polished “over” is difficult to bring back. Surprisingly, these nonnormal distributions have very little effect on Eq. 15.9 (if there are enough elements in the assembly). Thus, the situation is seen to be a complex one, but nonetheless one in which a little careful thought in relaxing tolerances to the greatest allowable extent can pay handsome dividends. For those who wish to avoid the labor of a detailed analysis, the use of Eq. 15.9, or even the assumption that the tolerance buildup will not exceed one-half or onethird of the possible maximum variation, are fairly safe procedures in assemblies of more than a few elements. Above all, when cost is important, one should try to establish tolerances which are readily held by normal shop practices. 15.3 Optical Mounting Techniques General. In optical systems, just as in precise mechanical devices, it is

best to observe the basic principles of kinematics. A body in space has six degrees of freedom (or ways in which it may move). These are translation along the three rectangular coordinate axes and rotation about these three axes. A body is fully constrained when each of these possible movements is singly prevented from occurring. If one of

576

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these motions is inhibited by more than one mechanism, then the body is overconstrained and one of two conditions occurs; either all but one of the (multiple) constraints are ineffective or the body (and/or the constraint) is deformed by the multiple constraint. The laboratory mount indicated in Fig. 15.9 is a classical example of a kinematic mount. Here it is desired to uniquely locate the upper piece with respect to the lower plate. At A the ball-ended rod fits into a conical depression in the plate. This (in combination with gravity or a springlike pressure at D) constrains the piece from any lateral translations. The V-groove at B eliminates two rotations, that about a vertical axis at A and that about the axis AC. The contact between the ball end and the plate at C eliminates the final rotation (about axis AB). Note that there are no extra constraints and that there are no critical tolerances. The distances AB, BC, and CA can vary widely without introducing any binding effects. There is one unique position which will be taken by the piece; the piece may be removed and replaced and will always assume exactly the same position. A perfectly kinematic system is frequently undesirable in practice and semikinematic methods are often used. These substitute smallarea contacts for the point and line contacts of a pure kinematic mount. This is necessary for two reasons. Materials are often not rigid enough to withstand point contact without deformation, and the wear on a point contact soon reduces it to an area contact in any case. Thus, in the design of an instrument, optical or otherwise, it is best to start by defining the degrees of freedom to be allowed and the degrees of constraint to be imposed. These can be outlined first by geometrical points and axes and then reduced to practical pads, bearings, and the like. This sort of approach results in a thorough and clear understanding of the effects of manufacturing tolerances on the function of the device and often indicates relatively inexpensive and simple methods by which a high order of precision can be maintained.

An example of a kinematic locating fixture. The three ball-ended legs of the stool rest in a conical hole at A, a Vgroove (aligned with A) at B, and on a flat surface at C. Figure 15.9

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577

Optical lens elements are almost always mounted in a close-fitting sleeve. A number of methods are used to retain the element in the mount; several are sketched in Fig. 15.10. In sketches (a) and (b) the lenses are retained by spring rings. In the left-hand mount (a), the spring catches in a V-groove, and if the mount is properly executed, the spring wire (which in its free state assumes a larger diameter) presses against the face of the element and the outer face of the groove. The lens is thus under a light pressure. The flat spring retainer (b) is less satisfactory, since the retainer will readily slip out unless the spring is strong or has sharp edges which bite into the mount. Other methods suitable for retaining low-precision elements include staking or upsetting ears of metal from the cell which clamp a thin metal washer over the lens element. Condenser systems are often mounted between three rods which are grooved as indicated in Fig. 15.10c. This provides a loose mount which leaves the condenser elements free to expand with the heat from the projection lamp without being constricted by the mount; it also allows cooling air to circulate freely. Both points are especially important in the mounting of a heat absorbing filter. Where precision is required, the cell is fitted rather closely to the lens. For good-quality optics the lens diameter may be toleranced 0.000, 0.001 in and the inside cell diameter toleranced 0.001, 0.000 in with 0.001 or 0.0005-in clearance between the nominal diameters. For small lenses which demand high precision, these tolerances can be halved, at the expense of some difficulty in production. Lens mounts.

Figure 15.10 Several methods of

retaining optical elements. (a) Wire spring ring in a V-groove; (b) flat spring ring; (c) three grooved rods at 120°; (d) and (e) threaded lock ring; (f) spinning shoulder, before burnishing and (dotted) after; (g) cemented in place with trough for cement overflow.

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Large-diameter optics are usually specified to somewhat looser tolerances. The lenses are most commonly retained by a threaded lock ring, as indicated in Fig. 15.10d or e. Sometimes the lock ring has an unthreaded pilot whose diameter is the same as the lens in order to be certain that the lens will ride on the bored seat and not on the threads. A separate spacer may be substituted for the pilot. The fit of the threaded parts should be loose so that the lens takes its orientation from the seat and shoulder, rather than from the threaded lock ring which frequently cocks. A lens may be spun into the mount, as shown in Fig. 15.10f. In this method the mount is made with a thin spinning shoulder which protrudes past the edge of the lens (which is preferably beveled). This spinning shoulder is a few thousandths of an inch thick at the outside edge and has an included angle of 10 or 20°. The lens is inserted and the thin lip is turned over, usually by rotating the cell while the lip is bent over. Care and skill are required, but there are a number of advantages to this technique. The pressure of the spinning shoulder tends to center the lens in the mount. In assemblies requiring extreme precision, the seat can be bored to fit the lens diameter and the lens can be spun in place without removing the piece from the lathe; the result is concentricity of an order which is difficult to duplicate by any other means. Another technique which results in both economy and precision is to cement the lens into its seat. The cement has a modest centering action, and with a good plastic cement the lens is securely retained. Care should be taken to provide an overflow groove (Fig. 15.10g) so that excess cement is kept away from the surface of the lens. For optics which must withstand a difficult thermal and/or vibration environment, a useful form of mount is achieved by making the inside diameter of the cell oversize and cementing the element in place with a compliant, elastomeric RTV type of cement. The lens is trued in the mount before it is cemented in place. This technique is especially useful for large-diameter elements where the thermal expansion difference between the element and the mount is a serious problem; the layer of RTV between the element and the cell is made thick enough to take up the expansion difference. In an assembly where several lenses and spacers are retained by a single lock ring, care must be taken that the thickness tolerances on the lenses and spacers are not allowed to build up to a point where the outside lens (1) extends beyond its seat and is not constrained by the seat diameter, or (2) is down into the mount so far that the lock ring cannot seat down on it. Another point to watch is that the mouth of a long inside-diameter bore is frequently bell-shaped, and a lens located near the mouth may have several thousandths of an inch more lateral

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579

(diametral) freedom than intended. In critical assemblies, it frequently pays to locate the lens well inside the mouth of the bore. When elements of different diameters are to be mounted together, the mount can be designed so that the lens seats can all be bored in one operation. This not only tends to reduce the cost of the mount but eliminates a possible source of decentration of each element with respect to the others, which can occur when the lens seats are bored in two or more separate operations. The microscope style of element mounting shown in Fig. 15.11 illustrates a number of valuable devices. The lens seat and the outside support diameter of each cell can be turned in the same operation; indeed, in a critical system, the optical element may be spun in place without removing the piece from the lathe. (Cementing the lenses in place can be substituted for spinning.) All the cells are seated in the same bore of the main mount and they are isolated from the lock-ring threads (not shown) by a long spacer. All these techniques contribute to maintaining the exquisite concentricity necessary in a first-class microscope objective. In mounting any type of optical element, it is important to avoid any warping or twisting. In the case of lens elements (which are in effect clamped between a shoulder and a lock ring, or their equivalents), this is not too difficult, since the pressure points are opposite each other and result in compression of the lens. More care is necessary in mounting mirrors and prisms, however, since it is quite easy to make the mistake of restraining a mirror in such a way that its surface is warped out of shape. One way to avoid this is to be sure that for each point at which pressure is exerted, there is a pad directly opposite so that no twisting moment is introduced. Figure 15.12 serves as an indication of how few constraints are necessary to kinematically define the location of a piece. This illustration might apply to a piece of cubical shape. The three points in the XZ plane define a plane on which the lower face of the piece rests; these points take up one translational and two rotational degrees of freedom. The two points in the YZ plane take up one translation and one

Mounting detail, microscope objective.

Figure 15.11

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Chapter Fifteen

Figure 15.12 Kinematic and semikinematic position defining mount for a rectangular

piece.

rotational freedom. Note that if there were three nonaligned points in this plane, they would then define an angle between the XZ and YZ faces of the piece; if the piece had a different angle, then there would be two ways in which the piece could be seated. The single point in the XY plane eliminates the last remaining of the six available degrees of freedom. A flexible pressure on the near corner of the piece will now uniquely locate the piece in this mount. The sketch on the right illustrates one way of putting this type of mount into practice. The points are replaced by pads or rails. As shown, the two rails in the XZ plane must be carefully machined in the same operation to assure that they are exactly coplanar: this is not difficult, but if it were, the substitution of a short pad for one rail would eliminate any difficulty on this score. Prisms and mirrors are usually clamped or bonded to their mounts. In clamp mounts the pressure is usually exerted by a screw on a metal pressure pad. A piece of cork or compressible composition material is placed between the glass and the metal pad to distribute the pressure evenly over the glass; this prevents the pressure from being exerted at a single point. There are a number of excellent cements available for bonding glass pieces to metal mounts. Some care is necessary in designing the mount when bonding a thin mirror, since the cement may warp the mirror (toward the shape of the mount) if the cemented area is large. 15.4

Optical Laboratory Practice

The lens bench. An optical bench or lens bench consists, in essence, of

a collimator which produces an infinitely distant image of a test target,

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a device for holding the optical system under test, a microscope for the examination of the image formed by the system, and a means for supporting these components. Each of the components may take various forms, depending on the usage for which it is primarily designed. The collimator consists of a well-corrected objective and an illuminated target at the focus of the objective. For visual work, the objective is usually a well-corrected achromat; for infrared work, a paraboloidal mirror is used, usually in an “off-axis” or Herschel configuration. The target may be a simple pinhole (for star tests or energy distribution studies), a resolution target, or a calibrated scale if a “focal” collimator is desired. The lens holder can range in complexity from a simple platform with wax to stick the lens in place to a T-bar nodal slide which generates a flat image surface. The microscope is usually equipped with at least one micrometer slide, and frequently with two or three orthogonal slides so that accurate measurements may be made. In subsequent paragraphs, we will discuss some of the applications of the lens bench and will describe the components of the bench more fully in the context of their applications. The measurement of focal length. There are two basic lens bench tech-

niques for the routine measurement of effective focal length: the nodal slide method and the focal collimator. Both schemes are sketched in Fig. 15.13. The nodal slide is a pivoted lens holder equipped with a slide which allows the lens to be shifted axially (i.e., longitudinally) with respect to the pivotal axis. Thus, by moving the lens forward or backward, the lens can be made to rotate about any desired point. Now note that, if the lens is pivoted about its second nodal point (as indicated in Fig.

Figure 15.13 Illustrating the nodal slide (upper) and the focal collimator

(lower) methods of measuring focal length on the optical bench.

582

Chapter Fifteen

15.13), the ray emerging from this point (which by definition emerges from the system parallel to its incoming direction) will coincide with the bench axis (through the nodal point). Thus there will be no lateral motion of the image when the lens is rotated about the second nodal point. Once the nodal point has been located in this manner, the lens is then realigned with the collimator axis and the location of the focal point is determined. Since the nodal points and principal points are coincident when a lens is in air, the distance from the nodal point to the focal point is the effective focal length. This technique is basic and applicable to a wide variety of systems. Its limitations are primarily in the location of the nodal point. The operation of swinging the lens, shifting its position, swinging again, and so on, is tedious, and since it is discontinuous, it is difficult to make an exact setting. If the axis of the test lens is not accurately centered over the axis of rotation of the nodal slide, there will be no position at which the image stands still. Lastly, the measurement of the distance from the axis of rotation to the position of the aerial image is subject to error unless the equipment is carefully calibrated. A focal collimator consists of an objective with a calibrated reticle at its focal point. The focal length of the objective and the size of the reticle must be accurately known. The test lens is set up and the size of the image formed by the lens is accurately measured with the measuring microscope. From Fig. 15.13 it is apparent that the focal length of the test lens is given by

冢 冣

F Fx  A′ 0 A

(15.10)

where A′ is the measured size of the image, A is the size of the reticle, and F0 is the focal length of the collimator objective. Note that the focal collimator may be used to measure negative focal lengths as well as positive; one simply uses a microscope objective with a working distance longer than the (negative) back focus of the lens under test. It is apparent from Eq. 15.10 that any inaccuracies in the values of A′, A, or F0 are reflected directly in the resultant value of the focal length. Further, any error in setting the longitudinal position of the measuring microscope at the focus will be reflected in Fx. Note that both the nodal slide and focal collimator methods assume that the test lens is free of distortion. If an appreciable amount of distortion exists, the measurements must be made over a small angle; this, of course, will limit the accuracy possible. In setting up a focal collimator, it is necessary to determine the collimator constant (F0/A) to as high a degree of accuracy as possible. The value of A, the reticle spacing, can be readily measured with a measuring microscope. The focal length of the collimating lens can be deter-

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583

mined to a high degree of accuracy by a finite conjugate version of the focal collimator technique. An accurate scale (or glass plate with a pair of lines) is set up 20 to 50 ft from the collimator lens, as shown in Fig. 15.14. The measuring microscope is used to measure the size of the image of the target accurately, and the distance from object to image is measured. The value of p, the distance between the principal points is estimated, either from the design data of the lens or by assuming it to be about one-third the lens (glass) thickness. (As long as p is small compared to D, the error introduced by an inaccurate value of p is small.) Now since D  s  s′  p and A:s  A′:s′, s and s′ can be determined and substituted (with due regard for the sign convention) into 1 1 1      (15.11) s′ f s and the value of the effective focal length determined. The necessity of estimating a value for p can be eliminated, if desired, by measuring the front focal length and applying the newtonian equation for magnification (Eq. 2.6) or, alternatively, by measuring front and back focal lengths (as outlined in the next paragraph), determining p  ffl  bfl  t  2f, and repeating the original calculation; after a few iterations the calculation will converge to the exact p and f. Collimation and the measurement of front and back focal lengths. A basic method of locating the focal points is by autocollimation. As indicated in Fig. 15.15, an illuminated target is placed near the focus of the lens

Figure 15.14 Setup for basic measurement of focal length.

Figure 15.15 Autocollimation as

a method of locating the focal points. When the object and reflected image are in the same plane (the focal plane), the system is autocollimated.

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under test and a plane mirror is placed in front of the lens so as to reflect the light back into the lens. When the reflected image is focused on a screen in the same plane as the target, both screen and target lie in the focal plane. For accurate work an autocollimating microscope, shown in Fig. 15.16, produces excellent results. The lamp and condenser illuminate the reticle, which may consist of clear lines scribed through an aluminized mirror. The reticle is then imaged at the focus of the microscope objective. The eyepiece of the microscope is positioned so that its focal plane is exactly conjugate with the reticle. Thus when the microscope is focused on the focal plane of the test lens, the reticle image is autocollimated by the test lens-plane mirror combination and is seen in sharp focus at the eyepiece. The microscope is then moved in to focus on the rear surface of the test lens; the distance traveled by the microscope is equal to the back focus of the lens. The lens bench collimator itself may be adjusted for exact collimation using this technique. When the collimator reticle and the reflected image of the microscope reticle are simultaneously in focus, then the collimator is in exact adjustment. Note that the mirror must be a precise plano surface if accurate results are expected. For routine measurements of back focus the bench collimator is substituted for the plane mirror, and if no autocollimating microscope is available, a little powder or a grease pencil mark on the rear surface of the test lens can be used as an aid in focusing on the lens surface. In the absence of many of the usual laboratory trappings, it is still possible to make reasonably accurate determinations of focal lengths and focal points. A lens may be collimated simply enough by focusing it on a distant object. The error in collimation can be determined by the newtonian equation x′  f 2/x, where x is the object distance less one focal length and x′ is the error in the determination of the focal position. A set of distant targets, such as building edges, smokestacks, and the like, whose angular separations are accurately known can often be substituted for a focal collimator in determining focal lengths.

Figure 15.16 The autocollimating microscope is used to

measure back focal length by focusing first on the surface of the test lens and then on the autocollimated image at the focal point.

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Measurement of telescopic power. The power of a telescopic system can be measured in three different ways. If the focal lengths of the objective and eyepiece (including any erectors) can be measured, their quotient equals the magnification. The ratio of the diameters of the entrance and exit pupils will also yield the magnifying power. Occasionally the multiplicity of stops in a telescope will introduce some confusion as to whether the pupils measured are indeed conjugates; in this case the image of a transparent scale laid across the objective can be measured at (or near) the exit pupil to determine the ratio. When the field of view is sharply defined, the magnification can be determined by taking the ratio of the tangents of the half-field angles at the eyepiece and the objective. Note that the almost inevitable distortion in telescopic eyepieces will usually cause this measurement of power to differ from measurements made by focal lengths or pupil diameters. One should ascertain that the telescope is in afocal adjustment before measuring the power. One way of doing this is to use a low-power (3 to 5) auxiliary telescope (or dioptometer) previously focused for infinity at the eyepiece; this reduces the effect of visual accommodation when the focus is adjusted. The measurement of aberrations. In most instances the aberrations of a

test lens can be readily measured on the lens bench by simulating a raytrace. For the measurement of spherical or chromatic aberration, a series of masks, each with a pair of small (to the order of a millimeter in diameter) holes, is useful. As indicated in Fig. 15.17, such a mask, centered over the test lens, simulates the passage of two “rays.” When the image is examined with a microscope, a double image of the target is seen, except when the microscope is focused at the intersection of the two rays. By measuring the relative longitudinal position of the ray intersections for masks of various hole spacings, the spherical aberration can be determined. If the measurements are made in red and blue light, the data will yield the chromatic and spherochromatic aberration of the lens. Figure 15.18 indicates how a similar three-hole mask can be used to measure the tangential coma of a test lens. A multiple hole mask can also be used to measure and plot a ray intercept curve, if desired. The

A two-hole mask can be used to locate the focus of a particular zone of a lens to determine the spherical aberration. Figure 15.17

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Figure 15.18 A three-hole mask

can be used to measure the coma of a test lens.

technique for measurement of field curvature is indicated in Fig. 15.19. The bench collimator is equipped with a reticle consisting of horizontal and vertical lines. The focal length of the test lens is measured. The lens is then adjusted so that its second nodal point is over the center of rotation of the nodal slide and the position of the focal point (with the lens axis parallel to the bench axis) is noted. The lens is then rotated through some angle . From Fig. 15.19 it is apparent that the intersection of the (flat) focal plane of the lens with the bench axis will shift away from the lens by an amount equal to 1 efl   1 cos 

冢

冣

as the lens is pivoted through an angle . The bench microscope is used to measure D, the amount by which the focus shifts along the axis. Two measurements are necessary, one for the sagittal focus and one for the tangential focus; this is the reason for the orthogonal line pattern of the reticle. Now the departure (along the bench axis) of the image surface from a flat plane is equal to 1 Defl   1 cos 

冢

冣

and the curvature of field (parallel to the lens axis) is given by 1 x  cos  D  efl   1 cos 

冤

冢

冣冥

Much of the numerical work in determining the field curvature by this method can be eliminated by the use of a T-bar attachment to the nodal slide. The cross bar of the T acts as a guide for the bench microscope, causing it to focus on the flat field position as the lens is pivoted. Thus one may measure the value of x/cos  directly; the use of the T-bar eliminates several sources of potential errors inherent in the method described above, although it does complicate the construction of the nodal slide. Measure at ± to detect a tilted field. Distortion is a difficult aberration to measure. The nodal slide may be used. The lens is adjusted on the slide so that no lateral image shift

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587

Figure 15.19 Geometry of the measurement of field curvature using

the lens bench nodal slide.

is produced by a small rotation of the lens. Then as the lens is pivoted through larger angles, any lateral displacement of the image is a measure of the distortion. An alternate method is to use the lens to project a rectilinear target and to measure the sag or curvature of the lines in the image, or to measure the magnification of targets of several different angular sizes. The difficulty with any method of measuring distortion is that one invariably winds up basing the work on measurements of magnification (or whatever) vanishingly close to the axis, and the accuracy of such small measurements is usually quite low. If the object imaged by a lens is effectively a “point,” i.e., if its nominal image size is smaller than the Airy disk, then the image will be a very close approximation to the diffraction pattern. A microscopic examination of such a “star” image can indicate a great deal about the lens to the experienced observer. One should be sure that the microscope NA is larger than that of the lens being tested. On the axis, the star image of a perfectly symmetrical (about the axis) system obviously must be a symmetrical pattern. Therefore, any asymmetry in the on-axis pattern is an indication of a lack of symmetry in the system. A flared or coma-shaped pattern on axis generally indicates a decentered or tilted element in the system. If the axial pattern is cruciform or shows indications of a dual focus, the cause may be axial astigmatism due either to a toroidal surface, a tilted or decentered element, or an index inhomogeneity. The axial pattern may also be used to determine the state of correction of spherical and chromatic aberration. The outer rings in the diffraction pattern of a well-corrected lens are relatively inconspicuous,

The star test.

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and the pattern, when defocused, looks the same both inside and outside the best focus point. In the presence of undercorrected spherical, the pattern will show rings inside the focus and will be blurred outside the focus; the reverse is true of overcorrected spherical. When the spherical aberration is a zonal residual, the ring pattern tends to be heavier and more pronounced than that from simple under- or overcorrected spherical. In the case of undercorrected chromatic, the pattern inside the focus will have a blue center and a red or orange outer flare. As the microscope focus is moved away from the lens, the center of the pattern may turn green, yellow, orange, and will finally become red with a blue halo. The reverse sequence will result from overcorrected chromatic. A chromatically “corrected” lens with a residual secondary spectrum usually shows a pattern with a characteristic yellow-green (apple green) center surrounded by a blue or purple halo. Off-axis star patterns are subject to a much wider range of variations. The classical comet-shaped coma pattern is easily recognized, as is the cross- or onion-shaped pattern due to astigmatism. However, it is rare to find a system with a “pure” pattern off-axis, and it is much more common to encounter a complex mixture of all the aberrations, which are difficult, if not impossible, to sort out. The star test is a very useful diagnostic tool requiring only minimal equipment, and, in skilled hands, it can be highly effective. The novice should be warned, however, that reliable judgments of relative quality are difficult, and a considerable amount of experience is necessary before one can safely depend on a star check for even simple comparative evaluations. It should not be used for quality control acceptance tests. The Foucault, or knife-edge, test is performed by moving a knife (or razor-blade) edge laterally into the image of a small point (or line) source. The eye, or a camera, is placed immediately behind the knife, and the exit pupil of the system is observed. The arrangement of the Foucault test is shown in Fig. 15.20. If the lens is perfect and the knife is slightly ahead of the focus, a straight shadow will move across the exit pupil in the same direction as the knife. When the knife is behind the focus, the direction of the shadow movement is the reverse of the knife direction. When the knife passes exactly through the focus, the entire pupil (of a perfect lens) is seen to darken uniformly. The same type of analysis can be applied to zones of the pupil. If a zone or ring of the pupil darkens suddenly and uniformly as the knife is advanced into the beam, then the knife is cutting the axis at the focus of that particular zone. This is the basis of most of the The Foucault test.

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589

Figure 15.20 The Foucault knife-edge test. Upper: On a perfect lens the

knife shadow has a straight edge. Lower: The shadow has a curved edge in the presence of spherical aberration. When the knife cuts through the focus, the pupil (or the zone of the focus) darkens uniformly.

quantitative measurements made with the Foucault test. The technique generally used is to place a mask over the lens with two symmetrically located apertures to define the zone to be measured. The knife is shifted longitudinally until it cuts off the light through both apertures simultaneously. It is then located at the focus for the zone defined by the mask. The process is repeated for other zones, and the measured positions of the knife are compared with the desired positions. This test is extremely useful in the manufacture of large concave mirrors, which can be tested either at their focus or at their center of curvature. For the center-of-curvature test, the source is a pinhole closely adjacent to the knife (Fig. 15.21), and a minimum of space and equipment is required. Obviously if the mirror is a sphere, all zones will have the same focus, and a perfect sphere will darken uniformly as the knife passes through the focus. When the surface to be tested is an aspheric, the desired foci for the various zones are computed from the design data and the measurements are compared with the calculated values. It is a relatively simple matter to convert these focus differences into errors in the surface contour; in this way the optician can determine which zones of the lens or mirror require further polishing to lower the surface. If the aspheric surface equation is expressed in the form

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Chapter Fifteen

Figure 15.21 The knife-edge test

applied to a concave mirror by placing both knife and source at the center of curvature.

x  f(y) then the equation of the normal to the surface at point (x1, y1) is y  y1  f(y1) f ′(y1)  xf ′(y1) [where f ′( )  dx/dy], and the intersection of the normal with the (optical) axis is then y1 x0  x1   f ′( y1) As an example, for a paraboloid represented by y2 x  4f y dx f ′(y)     dy 2f and the axial intersection of the normal through the point (x1, y1) is y1 y12 x0  x1    x1  2f    2f (y1/2f) 4f This last equation gives the longitudinal position at which the knife edge should uniformly darken a ring of semidiameter y1, when a parabola is tested at the center of curvature (as in Fig. 15.21) and knife and source are simultaneously moved along the axis. In practice, the knife edge is adjusted longitudinally until the central zone of the mirror darkens uniformly. The distance from the knife to mirror is then equal to 2f. Then a series of measurements is made using masks with half-spacings of y1, y2, y3, etc., each measurement yielding an error e1, e2, e3, etc., where e is the longitudinal distance from the “desired” position for the knife to the actual position. These data may be readily converted into the difference between the actual slope of the surface and the desired slope by reference to Fig. 15.22. When e is small, we can (to a very good approximation) write for our parabolic example

Optics in Practice

591

Figure 15.22 Geometry of knife-

edge test used to determine the surface contour of a concave (paraboloidal) mirror.

y A    e 兹苶 4f 2 苶 y2 where the term in the right-hand denominator is the distance from the surface to the axis taken along the normal. Now the angle  between the actual normal and the desired normal is equal to A    兹苶 4f 2 苶 y2 and substituting for A from the previous expression, we get ye   2 4f  y2 Note that  is also the amount by which the slope of the surface is in error; we can determine the actual departure of the surface from its desired shape by reference to Fig. 15.23. Taking the surface error at the axis as zero, the departure from the desired curve at y1 is given by y11 d1   2 At y2 it is 1 d2  d1   (y2  y1) (1  2) 2 At y3 it is 1 d3  d2   (y3  y2) (2  3) 2 In general we can write 1 in dn   冱 (yi1  yi) (i1  i) 2 i1

592

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where y0 and 0 are assumed zero, and the sign of d is positive if the actual surface is above (to the right in Figs. 15.22 and 15.23) the desired surface. The method outlined above can be readily applied to any concave aspheric. Since it checks the aspheric only at discrete intervals, it must, of course, be supplemented with an overall knife-edge check to be certain that the surface contour is smooth and free from ridges or grooves. The testing of convex surfaces is more difficult; they are usually checked in conjunction with another mirror chosen so that the combination has an accessible “center focus.” The computation of the normal is more involved in this case, but the principles involved are exactly the same. The Schlieren test. The Schlieren test is actually a modification of the

Foucault test in which the knife blade is replaced by a small pinhole. Thus any ray which misses the pinhole causes a darkened region in the aperture of the optical system. The Schlieren test is especially useful in detecting small variations in index of refraction, either in the optical system or in the medium (air) surrounding it. In wind-tunnel applications, the tunnel is set up between a collimating optical system and a matching system which focuses the image on the pinhole. When the test is recorded photographically, it is possible to derive quantitative data on the airflow from density measurements on the film. Resolution is usually measured by examining the image of a pattern of alternating bright and dark lines or bars. Conventionally, the bright and dark bars are of equal width. A target consisting of several sets of bar patterns of graded spacing is used, and Resolution tests.

Figure 15.23 Conversion of mea-

sured errors of surface slope () into the departure (d) of the actual surface from the desired surface.

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the finest pattern in which the bars can be distinguished (and in which the number of bars in the image is equal to the number in the object) is taken as the limiting resolution of the system under test. The resolution patterns in use vary in two details of (relatively minor) significance: the number of lines or bars per pattern and the length of the lines relative to their width. The most common practice is to use three bars (and two spaces) per pattern, with a length of five, or more, bar widths. The USAF 1951 target is of this type and the patterns are graded in frequency with a ratio of the sixth root of 2 between patterns. The National Bureau of Standards Circular No. 533 includes both high(25:1) and low- (1.6:1) contrast three-bar patterns which are approximately 1-in long and range in frequency from about one-third line per millimeter to about three lines per millimeter in steps of the fourth root of 2. A number of transparent (on film or glass) targets are commercially available; these are, for the most part, based on the USAF target. Figure 15.24 shows two types of resolution test targets. The USAF 1951 target is probably the most widely used and accepted resolution target. The radial target is interesting since it nicely demonstrates the 180° phase shift of the optical transfer function. This produces the “spurious resolution” which is illustrated in Fig. 15.24c. See also Figs. 11.16 and 11.17. In evaluating the resolution of a system it is important to adopt a rational criterion for deciding when a pattern is “resolved.” The following is strongly recommended: A pattern is resolved when the lines can be discerned, and when all coarser (lower-frequency) patterns also meet this requirement. This implicitly requires that the number of lines in the image be the same as in the target, and also rules out spurious resolution. Do not allow any consideration of “sharpness,” “definition,” “crispness,” “clearly resolved,” “contrast,” or the like to enter the evaluation; these are all subjective and involve individual interpretation. They lead to interminable arguments. The only consideration that should be used is “Can you discern the lines?”

Figure 15.24 (a) USAF1951 resolution chart; (b) Siemens star resolution chart; (c)

defocusing a well-corrected lens can cause a 180° phase shift which reverses the contrast of the pattern, causing areas which should be dark to be light and vice versa.

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The resolution of a photographic system is tested by photographing a suitable target and examining the film under a microscope. In order to obtain optimum results, the photographic processes must be carried out with extreme care, especially with regard to the selection of the best focus, exposure and development, and the elimination of any vibration in the system. If the microscope used in examination of the test film has a power approximately equal to the number of lines per millimeter in the pattern, the visual image will have a frequency equal to one line per millimeter and will be easy to view. Objective lenses can be tested on an optical bench with a resolution target in the collimator. For lenses with an appreciable angular coverage, an accurate T-bar nodal slide is practically a necessity if reliable offaxis results are to be obtained. Projection of a resolution target is a very convenient means of checking the resolution of lenses designed to cover areas less than a few inches in size. Care must be taken to ensure that the illumination system of the projector completely fills the aperture of the lens under test; otherwise, the results may be misleading. In all resolution tests, the alignment of the lens axis perpendicular to the target and film planes is a critical factor. The resolution of telescopic systems can be checked by visual observation of a suitably distant or collimated target. Since the limiting resolution of a telescope is frequently (by design) close to the limiting resolution of the eye, a common practice is to view the image through a low-power auxiliary telescope. Such a telescope serves a dual purpose in that it reduces the effect of the observer’s visual acuity on the measurement and also reduces the effect that involuntary accommodation (focusing) can have. The classical criterion for resolution, namely, the ability of a system to separate two point sources of equal intensity, is seldom used (except in astronomy). This is largely because a test using line objects is much easier to make. The measurement of the MTF (frequency response) is, in principle, quite straightforward. The basic elements of the equipment are shown in Fig. 15.25. The test pattern is one in which the brightness varies as a sinusoidal function of one dimension. Such a target is not an easy thing to prepare; fortunately the errors introduced by a target which is not truly sinusoidal are unimportant for most purposes. Some instruments utilize “squarewave” targets. The target pattern is imaged by the test lens on a narrow slit whose direction is exactly parallel to the target pattern. The light passing through the slit is measured by a photodetector. As the target or the slit is shifted laterally, the amount of light falling on the detector will vary, and the image modulation is given by Measurement of the modulation transfer function.

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Figure 15.25 The basic elements of modulation transfer (fre-

quency response) measurement equipment. The motion of the target scans its image across the narrow slit, where the maximum and minimum illumination levels are measured. By using targets of different spatial frequency, a plot of the modulation transfer function (vs. frequency) can be obtained.

max  min Mi   max  min where max and min represent the maximum and minimum illumination on the photodetector. The object modulation M0 is similarly derived from the maximum and minimum brightness levels of the target. The MTF (or frequency response, or sine-wave response, or contrast transfer) is then the ratio Mi : M0. A provision is usually made to vary the spatial frequency of the target pattern so that the response may be plotted against frequency. The target portion of the system may be as simple as a set of interchangeable targets which are slowly traversed by hand, or it may be a fully automatic device which translates the target and scans a range of frequencies simultaneously. The image-plane slit is almost never just a slit, since the manufacture of a slit of the required narrow dimensions can be fairly difficult. Instead, the image is magnified by a first-class microscope objective; this allows the use of a wider slit. Obviously any real slit width will have some effect on the measurements, and a slit as narrow as the sensitivity of the photodetector will allow should be used. The effect of the slit width on the response may be readily calculated, since it simply represents a line spread function of rectangular cross section, and the data can be adjusted accordingly where necessary.

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The source of illumination and the spectral response of the photodetector must, of course, be matched to the application for which the system under test is to be used. Otherwise, serious errors in measurement will result from the unwanted radiation outside the spectral band for which the system has been designed. Usually a set of filters can be found which will provide the proper response. Another technique which is much more widely used than that described above is based on a knife-edge scan. A knife edge is passed through the image of a point (or slit) and the light passing by the edge is measured. If the measured light I is plotted against the lateral position of the knife edge y, the slope of the curve (dI/dy) is exactly equal to the line spread function of the lens. The MTF can be calculated from the line spread function using the methods outlined in Secs. 11.8 and 11.9. Most commercial MTF equipment is set up so that the knife-edge scan data are read directly into a computer which processes the data to calculate the MTF at whatever frequency is desired. Note that this technique does not require a sinusoidal target, nor does it require a separate target for each frequency. As in any MTF measurement, the spectral distribution of the source and the response of the light-measurement sensor must match that of the application. The wave-front shape as measured by an interferometer can also be used to determine the MTF. The fringe pattern is scanned to digitize the data, and it is computer-processed to calculate the MTF at any desired frequency as in the knife-edge scan. This is entirely adequate for mirror systems or systems which operate at the laser wavelength. For systems which utilize a finite-width spectral band or a different wavelength, the results are not correct. The analysis of “unknown” optics. It is frequently necessary to deter-

mine the constructional parameters of an existing optical system. An example might be the analysis of a sample system to determine the reason for its failure to perform to the designer’s expectations. Another example might be the analysis of an existing lens so that its design data can be used as the starting point for a new design. For the most part this amounts to the measurement of the radii, thicknesses, spacings, and indices of the system components. Since the measurements to be made are frequently of a precision barely adequate for the purpose, it is best to provide as many interdependent checks on the process as possible. Thus the first steps should include accurate measurements of effective, back, and front focal lengths, as well as the aberrations, so that when all of the measured system data are collected, a calculation of the complete (measured) system can provide a final comparison check on the overall accuracy of the analysis.

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The thicknesses and spacings of a system are readily measured. For small systems a micrometer (equipped with ball tips for concave surfaces) is sufficient. A depth gage or an oversize plunger caliper (Nonius gage) is useful for larger systems. If a dimension can be deduced from two different measurements (as a check), the extra time involved is usually a worthwhile investment. The radius of an optical surface can be measured in many ways. The simplest is probably by use of a thin templet, or “brass gage,” cut to a known radius and pressed into contact with the surface. Differences between the gage and glass of a few ten-thousandths of an inch can easily be detected this way, but such a gage is not useful unless it very nearly matches the surface. The classical instrument for radius measurement is the spherometer, the basic principles of which are outlined in Fig. 15.26. The spherometer measures the sagittal height of the surface over a known diameter; the radius is determined from the formula Y2  S2 R   2S where Y is the semidiameter of the spherometer ring and S is the measured sagittal height. Since the sagittal height is a rather small dimension and thus subject to relatively large measurement errors, the accuracy of a spherometer leaves something to be desired even when extreme precautions are taken. One of the best ways to use a spherometer is as a comparison device, by measuring both the unknown radius and a (nearly equal) carefully calibrated standard radius (e.g., a test glass).

Figure 15.26 Left: Simple ring spherometer deter-

mines the radius of a surface through a measurement of the sagittal height. Right: The diopter gage or lens measure is a spherometer calibrated to read surface curvature in diopters.

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The diopter gage, or lens measure, or Geneva lens gage is a handy tool which can provide a quick approximate measure of the surface curvature. As shown in Fig. 15.26, it consists of a dial gage with its plunger between two fixed points. The dial of a diopter gage is calibrated in diopters; the readings may be converted to radii by the formula 525 R   millimeters D where the 525 is the constant representing 1000 (N  1) for an “average” opthalmic glass. The accuracy of a typical diopter gage is to the order of 0.1 diopter. Probably the best way to measure a concave radius is by use of an autocollimating microscope. The microscope is first focused on the surface and is then focused at the center of curvature (where the microscope reticle image is imaged back on itself by reflection from the surface). The distance traveled by the microscope between these two positions is equal to the radius. The precision of this method can be to the order of micrometers; the accuracy is obviously dependent on the accuracy of the measurement method used. If the microscope used is of fairly high power (say 150 with NA  0.3), the quality of the reflected image at the center of curvature is an excellent indication of the sphericity of the surface. Convex surfaces can be measured in this way provided that the working distance of the microscope objective is longer than the radius. A series of long-focal-length objectives is useful in this regard, although the precision of the method drops as the NA of the objective is lowered (long-focal-length objectives usually have a small NA) due to the increased depth of focus. If a precise determination of a long convex radius is necessary, a mating concave surface can be made so that it fits perfectly (as tested by interference rings) and the measurement is made on the concave glass. Master test plates are measured by this technique. Note that Eq. 15.3 can be used to calculate small radius differences from interference fringe readings. If a separate piece of glass from which the lens under analysis was made is available, the measurement of its index can be made with considerable precision. The minimum deviation of a test prism may be measured on a laboratory spectrometer, and the prism equations of Chap. 4 used to find the index. Alternatively, a Pulfrich refractometer measurement can be made. Either method will readily yield the index value accurate to the fourth decimal place. When one is constrained to measure the lens element itself, without destroying it, the problem is more difficult. A crude determination of the index can be made for normal glasses (i.e., not the newer “light” glasses) by measuring the density of the element. A plot of the catalog values of the index against density is then used to determine (very approximately) the corre-

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sponding index. The relationship between index (n) and density (D) is very approximately n  (11  D)/9. A somewhat more general method is to measure the axial thickness of the element and then to measure the apparent optical thickness by focusing a measuring autoreflecting microscope first on one surface and then the other. A simple paraxial calculation, taking into account the refractive properties of the surface radius through which the second surface is viewed, will yield a value for the index. Depending on the thickness of the element, the index value achieved will probably be almost completely unreliable in the third place, due to the large relative inaccuracy in the measurement of the apparent thickness and to the spherical aberration introduced by the thickness of the glass. If one measures the radii carefully and makes a good determination of the paraxial focal length of the element, the thick-lens formula for focal length can be solved to determine the index of refraction. Although this method requires skilled laboratory technique, it is capable of producing results which are accurate to one or two digits in the third place. Note that if care is not taken to eliminate the effects of spherical aberration from the focal-length measurement, the resulting index value will tend to err on the high side. Another nondestructive technique involves immersion in index-matching liquids, then measuring the index of the liquid.

Bibliography Note: Titles preceded by an asterisk (*) are out of print. Baird, K., and G. Hanes, in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 4, New York, Academic, 1967 (interferometers). DG-G-451, Flat and Corrugated Glass. *Deve, C., Optical Workshop Principles, London, Hilger, 1945. Habell, K., and A. Cox, Engineering Optics, London, Pitman, 1948. Hopkins, R., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, New York, Academic, 1980 (lens mounting). Ingalls, G., Amateur Telescope Making, books 1, 2, and 3, Scientific American, 1935, 1937, 1953. JAN-P-246 Slide Projectors. Malacara, D., “Optical Testing,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 30. Malacara, D., and Z. Malacara, “Optical Metrology,” in Handbook of Optics, vol. 2, New York, McGraw-Hill, 1995, Chap. 29. MIL-A-003920 Thermosetting Optical Cement. MIL-C-48497 Scratch and Dig for Opaque Coatings. MIL-C-675 Antireflection Coatings.

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MIL-G-1366 Aerial Photography Window Glass. MIL-G-16592 Plate Glass. MIL-L-19427 Anamorphic Projection Lenses. MIL-M-13508 Front Surface Aluminized Mirrors. MIL-O-13830 Scratch and Dig Specifications. MIL-O-16898 Packaging Optical Elements. MIL-P-47160 Optical Black Paint. MIL-P-49 16-mm Projectors. MIL-R-6771 Glass Reflectors, Gunsight. MIL-STD-1241 Optical Terms and Definitions. MIL-STD-150 Photographic Lenses. MIL-STD-34 Drawings for Optical Elements and Systems. MIL-STD-810 Interference Filters. McLeod and Sherwood, J. Opt. Soc. Am., vol. 35, 1945, pp. 136–138 (origin of the scratch and dig standards). Offner, A., Applied Optics, vol. 2, 1963, pp. 153–155 (null lens for parabola). Parks, R., “Optical Fabrication,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 40. Parks, R., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 10, San Diego, Academic, 1987 (fabrication). Photonics Buyers Guide, Optical Industry Directory, annually, Laurin Publishing Co., Pittsfield, Mass. Rhorer and Evans, “Fabrication of Optics by Diamond Turning,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 41. Sanger, G., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 10, San Diego, Academic, 1987 (fabrication, diamond turning). Scott, R., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965 (optical manufacturing). Shannon, R. R., “Optical Specifications,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 35. Shannon, R. R., “Tolerancing Techniques,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 36. Shannon, R., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 3, New York, Academic, 1965 (testing). Shannon, R., in Shannon and Wyant (eds.), Applied Optics and Optical Engineering, vol. 8, San Diego, Academic, 1980 (aspherics). *Strong, J., Procedures in Experimental Physics, Englewood Cliffs, N.J., Prentice-Hall, 1938. Strong, J., Procedures in Applied Optics, New York, Dekker, 1989. The Optical Industry Directory, Pittsfield, Mass., Photonics Spectra (published annually). Twyman, F., Prism and Lens Making, London, Hilger, 1988.

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Yoder, P. R., Mounting Lenses in Optical Systems, S.P.I.E., vol. TT21, 1995. Yoder, P. R., “Mounting Optical Components,” in Handbook of Optics, vol. 1, New York, McGraw-Hill, 1995, Chap. 37. Yoder, P., Opto-Mechanical System Design, New York, Dekker, 1986. Young, A., in Kingslake (ed.), Applied Optics and Optical Engineering, vol. 4, New York, Academic, 1967 (optical shop instruments). Zschommler, W., Precision Optical Glassworking, New York, Macmillan/S.P.I.E., 1984.

Index

Abbe prisms, 110–111 Abbe sine condition, 323 Abbe V- number, 94, 178 Aberrations, 61–62 astigmatism and field curvature, 69–71 (See also Astigmatism) balancing, 430–431 chromatic, 72–73 (See also Chromatic aberration) coma, 67–69 (See also Coma aberration) correction of, 80–83, 426–428 distortion, 71–72 (See also Distortion) lens shape and stop position effect on, 73–77 measurement of, 66–67, 585–587 optical computations for, 321–327 optical path difference, 79–80 (See also Optical path difference (OPD)) point spread functions for, 385–391 and ray intercept curves, 83–89 residual, 80–83, 429–430, 462 Seidel, 62–72 spherical, 64–67 (See also Spherical aberration) third-order (see Third-order aberrations) tolerances for, 355–359 variation with aperture and field, 77–79 zonal (see Zonal aberrations) Absorption, 173–178, 287 Absorption filters, 192–195 Acceptance cones, 282 Accommodation, 126, 131 Achromatic doublets, 412 Achromatic prisms, 94–96 Achromatic singlets, 415–417 Achromatic telescope objectives: design forms, 404–413 thin-lens theory for, 402–404

Additive tolerances, 570–575 Aerial image modulation (AIM) curves, 366–367 Afocal attachments, 470 Afocal systems, 251–255 Airspaced achromats, 408–409, 411 Airspaced anastigmats, 459–464 Airspaced triplets, 342–345, 506 Airy disks, 159 Alignment telescopes, 446 Alternate lenses in zoom systems, 295 Amici objective, 450–451 Amici prisms, 107–108 Anamorphic systems, 287–291 Angles: of diffraction, 382 of incidence, 7–8 of prisms, 95, 567–568 of refraction, 7–8 subtended, 251, 253, 268 Angstroms, 2–3 Angular aberrations, 66, 79 Angular blur, 154 Angular depth of focus, 155–156 Angular dispersion, 92 Angular field of view, 143, 253 Angular motion detection, 131 Angular resolution limits, 162 Angulon design, 470 Aniseikonina, 138 Antireflection coatings, 204 Apertures, 141–142 aberration effects of, 73–79 diffraction effects of, 157–160 in Galilean telescopes, 262 and image illumination, 151–154 in meniscus anastigmats, 454 in meniscus camera lens, 395, 397–399 and optical invariant, 54 603

604

Index

Apertures (Cont.): and pupils, 142–143 and sagittal coma, 323 and vignetting, 143–147 Aplanatic optical systems, 276 Aplanatic surfaces and fronts, 449–451 Apochromatic lenses, 411 doublets, 417–418 triplets, 505 Apodization, 380 Apparent angular field of view, 253 Apparent thickness, 29 Apparent width, 561 Aqueous humor, 126 Arc-lamp motion picture projectors, 472 Aspheric correctors, 486–487, 532, 541 Aspheric surfaces, 547 fabricating, 483–484, 557 general and skew rays on, 312–317 in meniscus camera lens, 400–401 plastic for, 190 for residual aberrations, 430 in third-order aberrations, 332–335 Astigmatism, 69–71, 76 computations for, 324 in Cooke triplets, 421 in eyes, 136 and field angle, 83 manual correction of, 427 in plane parallel plates, 103 with point spread functions, 385–386, 389, 391 in reflecting systems, 476–477 Astronomical telescopes, 252 Athermalization, 412–413 Autocollimating microscopes, 584, 598 Automatic computer design, 394, 431–435 Aviar lenses, 462 Axial gradients, 187 Back focal length, 23 calculation of, 39–40 and optical invariant, 53 of two-component systems, 47 in zoom systems, 294 Baffles, 148–150 Baker-Nunn satellite tracking cameras, 490 Balsam cement, 213 Bandpass filters, 207 Bang-bang zooms, 292 Bar targets, 366–367 Barium crowns and flints, 179 Barrel distortion, 72

Beaded screens, 197 Beam power, 165, 245 Beam splitter prisms, 103–104, 114–116 Beam truncation, 166 Beam waists, 165–168 Bell centering, 555 Bench collimators, 586 Binary surfaces, 296, 413 Binocular field of vision, 128 Binocular vision, lack of, 138 Binoculars, 258 Biocular systems, 444–445 Biotar objectives, 456, 459 Blackbody radiation, 231–237 Blanks, 549–550 Blind spot, 127 Blocking, 551–552 Blue optical glass filters, 193 Blur and blur sizes, 154–155 with Mangin mirrors, 487 rapid estimation of, 491–496 in reflecting systems, 476 with spherical aberrations, 364–365 Borosilicate glasses, 185 Bouwers system, 488–491 Brashear-Hastings prisms, 110–111 Brass gages, 597 Bravais system, 289 Brewster’s angle, 200 Brightness: conservation of, 227 telescope, 247 units for, 239 in visual acuity, 129–131 Broad-band coating, 205 Broken ring test, 128 Canada balsam, 213 Cancellation of waves, 11, 14 Candle power of searchlights, 245 Candles, 239 Cardinal points, 22–24 Cassegrain systems: benefits of, 482–483 conic sections in, 477–480 focal length in, 44–45 Schmidt, 487 Catadioptric systems, 487, 491, 533 Cataracts, 137 Cauchy dispersion equation, 176 Cemented doublets, 406–408 Cemented quadruplets, 436 Cemented triplets, 436 Cements, 213–214, 578, 580

Index Center-of-curvature tests, 589 Centering, 555–556, 565–567 Central negative doublets, 521 Central obscuration, 380–381 Chief rays, 69, 142 Chromatic aberrations, 72–73, 76–77 in blur, 492 in Bouwers system, 489–490 computations for, 325–326 in condenser systems, 472 in Cooke triplets, 420, 422 in eye, 137 in eyepieces, 440 in lens design, 433 manual correction of, 427 in plane parallel plates, 103 in prisms, 103 Rayleigh limit in, 358–359 residuals in, 81–82 in Schmidt systems, 485 in symmetrical principle, 401 in telescope objectives, 402 in visual acuity, 129–130 Chromatic difference of magnification, 73 Circular polarizers, 199 Cladding in fiber optics, 283–285 Closing equations, 302–303, 305 Coatings, 201–209 Coddington’s equations, 317–321 Coherent illumination, MTF with, 380–383 Cold mirrors, 210–211 Cold stops, 147–148 Collimators, 580–584, 586 Color in Cooke triplets, 420 Color temperature in blackbody radiation, 237 Coma aberration, 67–69 computations for, 322–323 in Cooke triplets, 421 in diffractive surface design, 417 in eyepieces, 440 and field angle, 83 and lens shape, 75–77 with Mangin mirrors, 487 manual correction of, 427 in plane parallel plates, 103 with point spread functions, 385, 388, 391 Rayleigh limit in, 358–359 in reflecting systems, 476–480 in symmetrical principle, 401 in telescope objectives, 402, 405–406 Communications, fiber optics for, 286–287 Comparison photometry, 132

605

Compensating eyepieces, 451 Compound microscopes, 269–271 Computer-controlled polishers, 558 Computer design, 431–435 Concave lenses, wave fronts affected by, 9 Concave radius: in microscope objectives, 452 in unknown optics analysis, 598 Concentric Bouwers, 489, 494–496, 498 Condenser systems, 245–247, 470–474 Cone channel condensers, 279–280 Cones, 127–128 Conic sections, 313, 484–485 Conjugates, 9, 251–252 Conrady dispersion equation, 176–177 Conservation of radiance, 225–230 Constant-deviation prisms, 105, 113–114 Contact lenses, 136–137 Contrast sensitivity, 132 Contrast transfer function, 369 Convergence, 131 Convex lenses, wave fronts affected by, 9 Convex radius in microscope objectives, 452 Cooke triplet anastigmats, 418–419 element shape solutions in, 421–422 glass choice in, 423–424 with high-index crowns, 511 initial aberration values in, 422–423 power and spacing solutions in, 419–421 Cooling process, 179 Corneas, 126 Cosine-to-the-fourth, 153–154 Cover glass in microscopes, 447 Critical angle in prisms, 96 Crown glasses, 179 in Cooke triplets, 418, 422–423, 511 in meniscus anastigmats, 457 in meniscus camera lenses, 395 in Petzval lenses, 467, 524 in telescope objectives, 402, 404–405 Crystalline materials, 187–188 Cup centering, 555 Curvature: Coddington’s equations for, 317, 319–320 computations for, 324 in meniscus camera lenses, 399 in paraxial raytracing, 37–38 Petzval (see Petzval curvature) in thin lenses, 42 Curves in design, 436 Cutoff frequencies, 377–378 Cylinder lenses, 287–289 Cylindrical surfaces, 557

606

Index

Dagors, 455, 516 Dall-Kirkham system, 481 Damped least squares, 434 Dark adaptation, 131–132 Data transmission, fiber optics for, 286–287 Defects, eye, 134–138 Density: of optical glass, 181 in transmission calculations, 175 Depolarizers, 200 Depth of field, 154 Depth of focus, 154–157, 348 Derotation prisms, 112 Detector optics, 274–281 Deviation: in centering, 565–566 in prisms, 91–92, 94 Dialyte achromats, 411 Diamond turning, 414, 483, 559 Dichroics, 210 Dielectric reflection, 200–209 Diffraction, 11–16 of apertures, 157–160 of gaussian beams, 163–168 Diffraction efficiency, 413–414 Diffraction grating, 163 Diffraction-limited systems, 376–383, 492 Diffractive surfaces, 296–297, 413 achromatic diffractive singlets, 415–417 apochromatic diffractive doublets, 417–418 diffraction efficiency in, 413–414 manufacturability of, 414 Sweatt model for, 414–415 Diffuse sources, irradiance from, 223–225 Diffusing materials, 195–198 Dimensions for prisms, 567–568 Diopter adjustments, 445 Diopter gages, 598 Diopters, 24, 125–126 Direct vision prisms, 94–96 Direction cosines, 308–311 Dispersing prisms, 91–92 Dispersion, 175–178 in fiber optics, 287 in prisms, 92 relative, 7 Distances: eye judgment of, 131 with microscopes, 447, 452 rangefinders for, 271–274 Distortion, 71–72, 76–77, 79 computations for, 324 in Cooke triplets, 421

Distortion (Cont.): in eyepieces, 440–441 keystone, 56–57 in lens design, 433 manual correction of, 427 measurement of, 586–587 in symmetrical principle, 401 Dogmar anastigmats, 462, 464, 517 Double-Gauss designs: anastigmats, 456, 459 camera lens, 537 high-index crowns, 534 high-speed lenses, 538 split-rear crowns, 536 Doublet magnifiers, 507 Doublet telescope objectives, 548 Dove prisms, 105–107 Dutch telescopes, 252 Effective clear aperture, 257–258 Effective focal length (efl), 23 calculation of, 39 and optical invariant, 53 in zoom systems, 294 Electromagnetic spectrum, 1–2 Electronic computer design, 431–435 Element shape solutions, 421–422 Ellipsoidal mirrors: in arc-lamp motion picture projectors, 472–473 manufacturing, 557 for reflecting systems, 477–484 Emissivity, 235–237 Empty magnification, 258 Endoscopes, 256–257 Enlarger lenses, 464 Entrance pupils, 52, 142, 254 Entrance windows, 143 Equiconcave and equiconvex elements, 436 Equivalent air paths, 257 Equivalent air thickness, 101 Erecting prism systems, 108–111 Erecting telescopes, 252, 254, 445 Erfle eyepieces, 444, 510 Exit pupils, 142 in magnifiers, 444 in optical devices, 257–267 in telescopes, 254, 260 Exit windows, 143 Express lenses, 455 Extended objects, 21 Eye relief, 254–255 Eyelenses: in microscopes, 269 in telescopes, 252–254

Index Eyepieces (see Telescope systems and eyepieces) Eyes, 125–126 defects of, 134–138 in optical design, 257–267 sensitivity of, 131–134 structure of, 126–128 visual acuity of, 128–130 F-numbers, 151–153 F-theta laser scanning lenses, 546 Farsightedness, 135–136 Fasteners, 213–214 Fiber optics, 281–285 for communications, 286–287 gradient, 285–286 Field, aberration variation with, 77–79 Field coverage, 424, 429 Field curvature, 69–71 Coddington’s equations for, 317, 319–320 computations for, 324 in meniscus camera lenses, 399 Field flatteners, 466–467 Field lenses, 255–257 light pipes for, 280 in radiometers, 278–279 Field of view: in field lenses, 255 in Galilean telescopes, 263 Field of vision, 128 Field stops, 141, 143 Fifth-order aberrations, 88, 352–354, 363–365 Filters: absorption, 192–195 interference, 200–209 photographic density of, 175 spatial, 168 thin-film coatings, 207 First-surface mirrors, 116–117 Fish-eye lenses, 468–469, 514 Fitting operations, 575 Flashed opal, 198 Flat-field microscope objectives, 451–452 Flint glasses, 179, 183 in Cooke triplets, 418 in meniscus anastigmats, 454, 457 in Petzval lenses, 467 in telescope objectives, 402 Float glass, 183 Focal collimators, 581–583 Focal lengths: in anamorphic systems, 288 in Cassegrain mirror systems, 44–45

607

Focal lengths (Cont.): Coddington’s equations for, 318 in compound microscopes, 269 measurement of, 581–584 and optical invariant, 53–54 in reflecting systems, 452, 479 in telescopes, 253 of thin lenses, 42 in two-component systems, 47–48 in zoom systems, 294–296 Focal points, 22 in image formation, 39–42 in telescopes, 252 Focus: in anamorphic systems, 289, 291 depth of, 154–157, 348 of eyepieces, 445 in optical path difference, 348–349 in zoom systems, 293 Foot-lamberts, 239 Foucault test, 557, 588–592 Fourier transform lenses, 168 Fovea, 127 Fraunhofer form, 405, 434 Frequency, 2 Frequency distribution curves, 570–572 Frequency response in MTF, 369 Fresnel lenses: plastics for, 191 in rangefinders, 274–275 Fresnel reflection, 200 Fresnel surfaces, 413 Front focal length (ffl), 23, 53 Front focus distance (ffd), 48 Front meniscus camera lenses, 400, 434 Fused fibers, 285 Fused quartz glass, 183, 185 G-sums, 339 Gain of projection screens, 197 Galilean telescopes, 252–253, 255 in anamorphic systems, 287–288 aperture stops in, 262 field of view in, 263 Gamma radiation, 1 Gastroscopes, 284 Gauss form: in lens design, 434 in telescope objectives, 405 Gaussian beams, diffraction of, 163–168 Gaussian optics, 22 Gelatin filters, 193 General and skew ray computations: aspheric surfaces, 312–317 spherical surfaces, 308–312

608

Index

Generalized design technique, 424 aberration balancing in, 430–431 manual correction in, 426–428 residual reduction in, 429–430 trigonometric correction in, 428–429 Generating process, 550 Geneva lens gages, 598 Geometric image energy distribution, 360–361 Geometric spot size, 362–366 Geometrical modulation transfer factor, 496 Germanium IR design, 544 Glare stops, 147–148 Glass fibers, 283–285 Glass filters, 194 Glass molding, 483–484 Glasses (see Optical glass) Goerz Dagors, 455 Goerz prisms, 111–112 Gradient index fibers, 285–286 Gradient index glasses, 187 Graphical raytracing, 306–307 Gray-bodies, 235 Green optical glass filters, 193 Gregorian telescopic system, 477–480 GRIN rods, 285–286 Grinding, 552–554, 556 Half-field angles in radiometers, 277 Hartmann dispersion equation, 176–177 Heat-absorbing glasses, 194 Height: for objects at infinity, 52 in raytracing, 38 Hektor anastigmats, 460–461 Heliar anastigmats, 460, 520 Hemispheres, radiation into, 222–223 Herzberger dispersion equation, 176–177 High-power microscope objectives, 450–451, 530 High-speed processing, 556 Higher-efficiency coating, 205 Higher-order aberrations, 88 Hot mirrors, 210 Huygenian eyepieces, 441 Huygen’s principle, 12, 157–158 Hyperboloids, 477–484 Hyperfocal distance, 156 Hypergon lenses, 401 Hyperopia, 135–136 Illumination: and apertures, 151–154 of natural sources, 239–240

Illumination (Cont.): in photometry, 240–242 units for, 239 in visual acuity, 129–131 Illumination devices: integrating spheres, 247–248 light pipes in, 281 projection condensers, 245–247 searchlights, 243–245 telescope brightness, 247 Image evaluation, 347 geometric spot size, 362–366 image energy distribution, 360–361 modulation transfer function, 366–372 computation of, 372–376 diffraction-limited systems, 376–383 optical path difference, 348–355 point spread functions for, 385–391 radial energy distribution, 383–385 spread functions for, 361–362 tolerances in, 355–360 Image formation, 21–22 cardinal points in, 22–24 focal points and principal points in, 39–42 light ray refraction in, 30–32 matrix optics in, 54–55 mirrors in, 43–45 optical invariant in, 49–54 paraxial raytracing in, 34–38 paraxial region in, 32–34 position in, 24–26 Scheimpflug condition in, 55–57 separated component systems in, 45–49 sign conventions in, 57–58 size in, 26–30 thin lenses in, 42–43 y-ybar diagrams in, 55 Image height: objects at infinity, 52 in paraxial raytracing, 38 Images: evaluating (see Image evaluation) forming (see Image formation) illumination of, 151–154 orientation of, in prism systems, 99–100, 105–107 radiometry of, 225–230 Immersion lenses, 277–280 Immersion objectives, 447, 450–451 Index dispersion, 175–178 Index-slope angle products, 37–38 Indexes: of eye surfaces, 127 of lenses in paraxial raytracing, 37–38

Index Indexes (Cont.): of prisms, 94 of refraction, 3–4 and dispersion, 178 importance of, 568 for mirrored surfaces, 43 test for, 592 Infinite conjugates, 251–252 Infinity, height for objects at, 52 Infinity f-numbers, 152–153 Infrared region, 1 Infrared transmitting glasses, 186–187 Instrument myopia, 135 Integrating spheres, 200, 247–248 Intensity: in photometry, 240 in radiometry, 220–221 Intercept length for mirrored surfaces, 44 Interference, 11–16 Interference coatings, 207–208 Interference filters, 200–209 Interferometers, 558 Internal transmittance, 184 Intersection coordinates for skew rays, 313–314 Inverse Dall-Kirkham system, 481 Inverse square law, 220–221 Inversion prisms, 111–113 Inverting telescopes, 252 IR Cooke triplet, 543 IR telescope, 545 Iris, 126 Irradiance: from diffuse sources, 223–225 in photometry, 240–242 in radiometry, 220 Iterative technique, 428 Johnson’s law, 376 K-mirrors, 113 Kellner eyepieces, 442 Kepler telescopes, 254–255 Keratoconus, 137 Kettler-Drude dispersion equation, 176–177 Keystone distortion, 56–57 Kinematic mounts, 575–576 Kinoforms, 296, 413 Knife-edge scans, 596 Knife-edge test, 588–592 Knife-edge traces, 362 Knoop hardness, 181 Koehler projection condensers, 471 Koenig prisms, 110–111

609

Lagrange invariant, 49–54 Lambertian diffusers, 195–196 Lamberts, 239 Lambert’s law, 221–222 Landolt broken ring test, 128 Laser ablation, 136–137 Laser beam diffraction, 163–168 Laser beam expanders, 255 Laser diodes, 291 Laser disk objectives, 547 Laser rangefinders, 274 LASIK, 136–137 Lateral aberrations, 64–66, 322, 358 Lateral magnification, 26 Law of refraction, 5–8 Laws of probability, 570 Leman prisms, 111–112 Lens bench collimators, 584 Lens benches, 580–581 Lens shape effect on aberrations, 73–77 Lenses: designs for: automatic, 432–435 sample, 503–548 mounts for, 577–580 power of, 24 in unknown optics analysis, 598 wave fronts affected by, 8–11 Lenticular screens, 197 Licht-Sprechers, 97 Light pipes, 279–281 Light wave propagation, 2–5, 157–158 Line images, 289–290 Line spread functions, 361–362 Linear aberrations, 79 Linear blur, 154 Linear dimensions in computations, 302 Linear kinoform surfaces, 413 Linear resolution, 163 Liquids, 213–214 Long-pass transmission filters, 207 Longitudinal departure, 71 Longitudinal magnification, 27 Longitudinal spherical aberrations, 64–66, 322 Lord Rayleigh’s criterion, 161–162 Low-expansion glasses, 185–186 Low-index, broadband Cooke triplets, 512 Low-index glass, 527 Low-power microscope objectives, 448 Low-reflection coatings, 204–205 Lumens, 219, 237–239 Luminous radiation, 237–243 Lyot stops, 147

610

Index

Magnetorheologic polishing, 558 Magnification, 26–27 in anamorphic systems, 287 in microscopes, 269–270 in telescopes, 251, 253–254 Magnifiers, 267–269, 285, 444–445 Maksutov system, 486–491 Mangin mirrors, 487–488, 493–494, 497 Manual aberration correction, 426–428 Marechal criterion, 357, 385, 387 Materials: in design, 435 in optical manufacture, 549–550 specifications and tolerances for, 568–569 Matrix optics, 54–55 Measurements: aberration, 66–67, 585–587 focal length, 581–584 modulation transfer function, 594–596 telescopic power, 585 Medium-power microscope objectives, 448–449 Melt fits, 575 Meniscus forms: camera lens, 395–401 in design, 436 focal points in, 41 inner crown, 529 for photographic objectives, 453–459 in residual aberrations, 429 Meridional rays and planes, 69, 304–308 Merit function, 432–434 Merte effect, 462 Merte surfaces, 460 Mesopic curve, 134 Micrometers, 2–3 Microns, 2–3 Microscopes and microscope objectives, 447–448 aplanatic surfaces in, 449–450 autocollimating, 584, 598 compound, 269–271 flat-field, 451–452 high-power, 450–451, 530 low-power, 448 medium-power, 448–449 Rayleigh limit in, 358 reflecting, 452–453 simple, 267–269 Millimicrons, 2–3 Minifiers, 285

Minimum deviation of prisms, 94 Mirrors: ellipsoidal, 472–473, 477–484, 557 in image formation, 43–45 Mangin, 487–488, 493–494, 497 mounting, 580 plane, 116–117 semireflecting, 210 spherical, 474–476, 493, 497 Modified Amici prisms, 111–112 Modulation transfer function (MTF), 366–372 with coherent and semi-coherent illumination, 380–383 computation of, 372–376 diffraction-limited systems in, 376–383 measurement of, 594–596 Motion, magnification of, 27 Mounting techniques, 575–580 Multilayer coatings, 207–209 Myopia, 134–135 Nanometers, 2–3 Narrow bandpass filters, 207 Natural stop positions, 76 Nearsightedness, 134–135 Negative magnification, 27 Negative outer meniscus elements, 539 Newton’s black spot, 15 Newton’s rings, 14–15 Nicol prisms, 199 Night myopia, 135 Nodal points, 22–23 Nodal slides, 581 Nonbrowning glasses, 183 Nonspherical surfaces, 557–559 Null lenses, 558 Numerical aperture (NA), 152 in fiber optics, 282 in illumination for MTF, 382–383 Objective lenses and systems: in microscopes, 269, 447–453 photographic (see Photographic objectives) in telescopes, 252, 254, 402–413, 445–447 testing, 594 Offense against sine condition (OSC), 323 Oil-immersion microscopes, 450 Old Schott dispersion equation, 176–177 1-diopter prisms, 126 Opal glass, 198, 200

Index Opening equations, 302, 304–305, 309, 319 Optic nerve, 127 Optical axes, 22 Optical coatings, 201–209 Optical computations, 301–302 aberration, 321–327 Coddington’s equations, 317–321 general and skew rays: aspheric surfaces, 312–317 spherical surfaces, 308–312 meridional rays, 304–308 paraxial rays, 302–304 Optical contact method, 214 Optical devices, 251 anamorphic systems, 287–291 compound microscopes, 269–271 diffractive surfaces, 296–297 exit pupils, eyes, and resolution in, 257–267 fiber optics, 281–287 field lenses and relay systems, 255–257 radiometers and detector optics, 274–281 rangefinders, 271–274 simple microscopes and magnifiers, 267–269 telescopes, 251–255 variable-power systems, 291–296 Optical glass, 178–184 in Cooke triplets, 418, 422–424, 511 gradient index, 187 infrared transmitting, 186–187 low-expansion, 185–186 in meniscus anastigmats, 454, 457 in meniscus camera lenses, 395 in Petzval lenses, 467, 524 in telescope objectives, 402, 404–405, 410 Optical invariant, 49–54 Optical laboratory practice: aberration measurement, 585–587 focal length measurement, 581–584 Foucault test, 588–592 lens benches, 580–581 modulation transfer function measurement, 594–596 resolution tests, 592–594 Schlieren test, 592 star test, 587–588 telescopic power measurement, 585 unknown optics analysis, 596–599 Optical manufacture: blocking, 551–552 centering, 555–556 grinding, 552–554

611

Optical manufacture (Cont.): high-speed processing, 556 materials, 549–550 nonspherical surfaces, 557–559 polishing, 554–555 rough shaping, 550–551 single-point diamond turning, 559 Optical mounting techniques, 575–580 Optical path difference (OPD), 15, 79–80 for aberration measurements, 66–67 computations for, 326–327 focus shift in, 348–349 in ray intercept plots, 88–89 RMS, 355–356 spherical aberration in, 349–355 Optical path length, 15 Optical specifications and tolerances, 559–560 additive, 570–575 centering, 565–567 materials, 568–569 prism dimensions and angles, 567–568 surface accuracy, 560–564 surface quality, 560–561 thickness, 564–565 Optical systems, resolution of, 160–163 Optical systems design, 393–395 achromatic telescope objectives, 402–413 Cooke triplet anastigmats, 418–424 diffractive surfaces, 413–418 by electronic computer, 431–435 generalized design technique, `424–431 practical considerations in, 435–436 simple meniscus camera lens, 395–401 symmetrical principle in, 401 Optical transfer function (OTF), 372 Orders of aberrations, 83–89 Orientation in prism systems, 99–100, 105–107 Orthometar lenses, 455 Orthoscopic eyepieces, 442–443 OSC aberration computations, 323 Overcorrected astigmatism, 71 Overcorrected distortion, 72 Overcorrected spherical aberration, 65 Overspecification, 559 Paraboloidal mirrors: blur size estimation in, 493 manufacturing, 557 in reflecting systems, 476–477

612

Index

Paraxial rays: computations for, 302–304 for mirrored surfaces, 43 through several surfaces, 34–38 in third-order aberrations, 329 Paraxial region, 22, 32–34 Path length in fiber optics, 282 Pattern-generating surfaces, 297 Peak-to-valley (P-V) OPD, 356 Peaking-up characteristics, 572–573 Pechan prisms, 112 Pellicles, 114–115 Penta prisms, 113–114 Pentac anastigmats, 460 Perfect optical systems, 22 Periscopes, 256–257, 401 Petzval curvature, 70–71 in Cooke triplets, 418, 422 in eyepieces, 440 manual correction of, 427 in meniscus camera lens, 395–396, 400 Petzval lenses: for photographic objectives, 465–467 with split elements, 522, 524 Petzval sum, 420 Petzval surfaces, 71, 423 Phase shifts, 287, 379 Phase transfer function (PTF), 372 Photoelectric effect, 16–17 Photographic density of filters, 175 Photographic depth of focus, 156–157 Photographic objectives, 453 afocal attachments, 470 airspaced anastigmats, 459–464 meniscus anastigmats, 453–459 Petzval lenses, 465–467 reverse telephoto lenses, 468–470 telephoto lenses, 467–468 Photographic triplet lens, 342–345 Photometry, 219–220, 237–243 Photopic curve, 134 Pincushion distortion, 72, 440 Pipes, light, 279–280 Pitch in blocking, 551 Planck’s law, 232–235 Plane mirrors, 116–117 Plane parallel plates, 100–104 Plane surface reflections, 97–100 Plane waves, 2 Plasmat lenses, 455 Plastic cements, 214 Plastic fibers, 283–285 Plastic optical materials, 188–192 Plate glass, 183

Ploessl eyepieces, 443–444, 509 Point spread functions (PSFs), 361–362, 385–391 Polarizing materials, 197–200, 209 Polishing, 554–556, 558 Porro prisms, 109–110 Portrait lenses, 465 Position in image formation, 24–26 Power: in anamorphic systems, 287, 289 in Cooke triplet anastigmats, 419–421 in design, 426 of field lenses, 261–262 of lenses, 24 of microscopes, 267–270 radiated into hemispheres, 222–223 of searchlights, 245 in telescopes, 251, 253, 259, 263–267, 585 of two-component systems, 47 Precision bevels, 436 Precision in computations, 301–302 Presbyopia, 137 Pressing, 549 Primary aberrations, 64 manual correction of, 426–428 point spread functions for, 385–391 Principal planes, 45–46 Principal points, 22, 39–42 Principal rays, 69, 142, 329 Prisms, 91 achromatic and direct vision, 94–96 in anamorphic systems, 287, 290–291 designing, 117–122 dimensions and angles for, 95, 567–568 diopter, 126 dispersing, 91–92 erecting systems for, 108–111 in eyepieces, 440 inversion, 111–113 minimum deviation of, 94 mounting, 580 Penta, 113–114 plane parallel plates in, 100–104 polarizing, 199 in rangefinders, 272–273 reflection from plane surfaces in, 97–100 rhomboids and beam splitters, 114–116 right-angle, 104–107 roof, 107–108 thin, 92–94 total internal reflection in, 96–97 wave fronts affected by, 8–11 PRK technique, 136

Index Projection condensers, 245–247, 470–471 Projection screens, 195–198 Projection TV objectives, 542 Protars, 454 Protected glasses, 183 Pulfrich refractometers, 598 Pupils: and aperture stop, 142–143 eye, 126 in magnifiers, 444 in optical devices, 257–267 in telescopes, 254, 260 zones of, 588–589 Purkinje shift, 134 Purple optical glass filters, 194 R-Biotars, 525 Radial energy distribution, 383–385 Radial gradients, 187 Radial keratotomy, 136 Radial test targets, 593 Radiant intensity, 240 Radiation: blackbody, 231–237 glasses for, 183 into hemispheres, 222–223 reducing, 148–150 Radiometers, 274–281 Radiometry and radiance, 219–220 blackbody radiation, 231–237 conservation of, 225–230 and diffuse sources, 223–225 and hemispheres, 222–223 of images, 225–230 inverse square law for, 220–221 and Lambert’s law, 221–222 spectral, 230–231 Radius in unknown optics analysis, 597 Ramsden eyepieces, 441–442 Rangefinders, 271–274 Rapid estimation of blur size, 491–496 Rare earth glasses, 179, 183, 423 Ray heights in raytracing, 37–38 Ray refraction at single surface, 30–32 Ray slope-index product, 319 Rayleigh limit (RL), 355–357 Rayleigh’s criterion, 161–162 Rays, 4 intercept curves for, 65, 83–89 through lenses, 10 meridional, 69, 304–308 paraxial (see Paraxial rays)

613

Raytracing: in aberration measurements, 585 computer effects on, 394 graphical, 306–307 in optical computations, 302 through several surfaces, 34–38 for spot diagrams, 360–361 Real angular field of view, 253 Real images, 10 Rear meniscus camera lens, 400, 434 Rear projection screens, 198 Reciprocal relative dispersion, 93–94, 178 Red optical glass filters, 194 Reduction of residual aberrations, 429–430 Reflectance levels of natural sources, 239–240 Reflecting microscope objectives, 452–453 Reflecting systems, 474 Bouwers system, 488–491 conic sections through origins in, 484–485 ellipsoid and hyperboloid, 477–484 Mangin mirrors, 487–488 paraboloidal reflectors in, 476–477 Schmidt system, 485–487 spherical mirrors in, 474–476 Reflection, 173–175 dielectric, 200–209 in fiber optics, 282 with immersion lenses, 278 in prisms, 96–100 Reflectors, 117–122, 209–211 Refracting prisms, 290–291 Refraction: equations for, 302, 305, 309 law of, 5–8 at single surface, 30–32 for skew rays, 315–317 Regions of solution, 427–428 Reinforced waves, 14 Relative apertures, 152 Relative dispersion, 7, 178 Relay systems, 256–257 Replication, plastics for, 191 Residual aberrations, 80–83, 429–430, 462 Resistance of optical glass, 181 Resolution: of compound microscopes, 270–271 in diffraction-limited systems, 379 of eyes, 258 in fiber optics, 283 in modulation transfer function, 367–368, 376 in optical devices, 257–267

614

Index

Resolution (Cont.): of optical systems, 160–163 tests for, 592–594 Reticles, 211–213 Retina, 127–128 Retrofocus lenses, 468–470, 513 Reverse telephoto lenses, 468–470, 513 Reversed Tessars, 519 Rhomboid prisms, 114–116 Right-angle prisms, 104–107 Ritchey-Chretien objective, 479–480 RMS (root-mean square) OPD, 355–356 Rod-lens endoscopes, 257 Rods, 127–128 Ronchi grating tests, 557 Roof prisms, 107–108, 112 Rough shaping, 550–551 Sagittal coma, 69, 103, 323 Sagittal curvature of field, 317 Sagittal height, 16 Scaling of aberrations, 79 Scheimpflug condition, 55–57 Schlieren test, 592 Schmidt cameras, 333 Schmidt prisms, 111–112 Schmidt systems: blur size estimation in, 493, 498 Cassegrains, 487 in reflecting systems, 485–487 Schwarzchild configuration, 452 Scotopic curve, 134 Scratch and dig specifications, 436 Searchlights, 243–247 Second-surface mirrors, 116–117 Secondary spectrum (SS), 82 in achromatic telescope objectives, 409–410 in diffractive surface design, 416 Seidel aberrations, 62–72 Seidel coefficients, 331 SELFOC rods, 285 Sellmeier dispersion equation, 176–177 Semi-coherent illumination, MTF with, 380–383 Semireflecting mirrors, 210 Sensitivity of eyes, 131–134 Separated component systems, 45–49 Seventh-order aberrations, 88 Sheet polarizers, 199 Short-pass transmission filters, 207 Sigmoidoscopes, 284 Sign conventions, 25, 30–31, 57–58 for mirrored surfaces, 43 for telescopes, 253

Simple lenses: blur size estimation in, 494 meniscus camera, 395–401 wave fronts affected by, 8–11 Simple microscopes, 267–269 Simultaneous design techniques, 432 Sine wave response, 369 Sine-wave targets in MTF, 375–376 Single-lens elements, blur size estimation in, 499 Single-lens reflex (SLR) cameras, 274 Single-material catadioptric systems, 533 Single-point diamond turning, 414, 483, 559 Single refracting elements, blur size estimation in, 498 Single surface, ray refraction at, 30–32 Singlet correctors, 531 Size in image formation, 26–30 Skew rays, 69 aspheric surface computations, 312–317 spherical surface computations, 308–312 Slits in MTF tests, 594–596 Slope angles in paraxial raytracing, 38 Snell’s law of refraction, 5–8 Sonnar anastigmats, 456, 528 Spacing: in Cooke triplet anastigmats, 419–421 in design, 426 in microscope objectives, 452 in telescopes, 263–265 in unknown optics analysis, 597 Sparrow’s criterion, 160 Spatial filtering, 168 Special glasses: gradient index, 187 infrared transmitting, 186–187 low-expansion, 185–186 Spectral radiometry, 230–231 Speed of systems, 152 Spheres, integrating, 247–248 Spherical aberration, 64–67 in anastigmats, 424, 458, 461 in blur, 364–365, 492 computations for, 322 in condenser systems, 472 in Cooke triplets, 421–422 in diffraction-limited systems, 379–381 in diffractive surface design, 416 in eyepieces, 440 fifth-order, 352–354 geometric spot size due to, 362–366 and lens shape, 75 manual correction of, 427 in meniscus camera lens, 395, 399

Index Spherical aberration (Cont.): in optical path difference, 349–355 in Petzval lenses, 467 in plane parallel plates, 103 in point spread functions, 386–387, 390–391 Rayleigh limit in, 358 in reflecting systems, 474–476, 479–480 in telescope objectives, 402, 405–409 third-order, 335, 351–352 wave aberration polynomial for, 354–355 Spherical gradients, 187 Spherical mirrors, 474–476, 493, 497 Spherical reflectors, 473 Spherical surfaces, general and skew rays on, 308–312 Spherical test plates, 561 Spherochromatism, 82 computations for, 325 in diffractive surface design, 416 in residual aberrations, 429 in telescope objectives, 406–409 Spherometers, 597 Spike filters, 207 Spinning shoulders, 578 Split elements, 462–463 Split-front triplets, 526, 529 Split-image rangefinders, 274 Split-rear crown double Gauss, 536 Spot diagrams, 360–361 Spot size due to spherical aberration, 362–366 Spread functions, 361–362 Spreading of gaussian beams, 165–166 Sprenger prisms, 112 Spurious resolution, 379 Square-wave targets in MTF, 375–376 Star test, 587–588 Statistical combination, 570 Stefan-Boltzmann law, 232, 235 Steinheil form, 405 Steradians, 220 Stereo vision, 131 Stokes lenses, 289 Stop shift equations, 335–345 Stops (see Apertures) Stray radiation, 148–150 Strehl definition, 368 Strehl ratio, 356–359, 385 Styrene plastic, 191 Subtended angles, 251, 253, 268 Superachromat lenses, 411 Surface curvature in eye, 127

615

Surfaces: diffractive, 296–297 specifications and tolerances for, 560–564 in third-order aberration computations, 328–335 Surveying instruments, 258, 446 Sweatt model, 414–415 Symmetrical eyepieces, 443–444, 509 Symmetrical principle, 401 Synthesis of optical systems (see Optical systems design) Systems of separated components, 45–49 T-stops, 153 Tangential coma, 69, 322–323, 358, 417 Tangential curvature of field, 317 Tangential images, 69 Tangential rays and planes, 69 Targets in MTF, 366–367, 375–376 Telecentric stops, 150–151 Telephoto lenses, 467–468, 515 Telephoto ratio, 467 Telescope systems and eyepieces, 251–255, 439–441, 508 brightness in, 247 diopter adjustment of, 445 erector systems, 445 Erfle eyepieces, 444 Huygenian eyepieces, 441 Kellner eyepieces, 442 magnification, 52 magnifiers, 444–445 objective systems in, 252, 254, 402–413, 445–447 orthoscopic eyepieces, 442–443 power measurements, 251, 253, 259, 263–267, 585 Ramsden eyepieces, 441–442 Rayleigh limit in, 358 symmetrical eyepieces, 443–444 Temperature: in blackbody radiation, 232, 234 and telescope objectives, 412 Terrestrial telescopes, 252 Tessar anastigmats, 459, 518 Test plates, 561, 574 Theodolites, 446 Thick lenses: in Cooke triplets, 422 in design, 435–436 Thickness, 564–565 apparent, 29 of filters, 194 magnification of, 27

616

Index

Thickness (Cont.): in paraxial raytracing, 37–38 in unknown optics analysis, 597 Thickness fits, 575 Thin elements, 435 Thin-edged elements, 435 Thin-film computations, 205–209 Thin lenses: aberration expressions, 428 blur size estimation in, 494, 500 in image formation, 42–43 stop shift equations, 335–345 for telescope objectives, 402–404 Thin prisms, 92–94 Third-order aberrations, 64, 88, 351–352 in Cooke triplets, 422 in diffraction-limited systems, 379–381 in geometric spot size, 362–363 in meniscus camera lenses, 396–398 Rayleigh limit in, 358 in reflecting systems, 479–480 in residual aberrations, 429 surface contribution in, 328–335 thin lenses, 335–345 Third-order theory, 88 35-mm camera objectives, 535 Three-dimensional vision, 131 Three-hole masks, 585–586 Topogon lens, 454 Toroids, 557 Total curvature of thin lenses, 42 Total emissivity, 235–236 Total internal reflection (TIR), 96–97, 283–284 Transfer equations, 302–303, 305, 309, 311 Transformation temperature in glass, 181 Transmission: calculations for, 174–175 in radiance of images, 226 Transmitting diffusers, 197–198 Transverse aberrations, 64–66, 322, 358 Transverse magnification, 26 Triangulation rangefinders, 271 Trigonometric correction, 428–429 Trigonometric functions, 301–302 Triplet achromats, 410 Triplets: with aspheric field correctors, 541 Cooke (see Cooke triplet anastigmats) Truncation, beam, 166 Tunnel diagrams, 105 Twisting in lens mounting, 579 Two-component systems, 47–49

Ultraviolet region, 2 Undercorrected astigmatism, 70 Undercorrected spherical aberrations, 65 Underspecification, 559–560 Unfolding prisms, 104–105 Unknown optics analysis, 596–599 USAF1951 resolution test target, 593 V-number, 94, 178–179, 183 Variable-power systems, 291–296 Velocity of propagation, 3 Vernier acuity, 131 Vertex length, 424, 456 Viewer lenses, 444–445 Vignetting, 143–147 Virtual images, 10 Visible spectrum, 1 Visual acuity, 128–130 Visual centering, 555 Visual resolution of microscopes, 270–271 Vitreous humor, 126 Waists, 165–168 Warping in lens mounting, 579 Watts, 219 Wave aberration polynomial, 354–355 Wave fronts: aberration, 79–80, 88–89, 326–327 simple lens and prism affects on, 8–11 Wavelength, 1–3 in blackbody radiation, 232–234 and dispersion, 176 and emissivity, 236 and eye sensitivity, 133–134 in fiber optics, 287 in radiometry, 219 Wide-angle design, 539 Wide-angle lenses, 154 Wide-angle photography, 455 Widely airspaced doublets, 411 Wien’s displacement law, 232, 235 Wind-tunnel applications, 592 Window glass, 183 Wood lenses, 286 Working f-numbers, 152 Wratten filters, 193 Y-ybar diagrams, 55 Ynu raytraces, 34 Young’s experiment, 12–13, 15 Zeiss Protars, 454 Zero-power meniscus elements, 429

Index Zonal aberrations, 81 in anastigmats, 424 computations for, 322 in diffractive surface design, 416 with point spread functions, 390 Rayleigh limit in, 358

Zonal aberrations (Cont.): in residual aberrations, 429 in telescope objectives, 407–409 Zones of pupils, 588–589 Zoom systems, 291–296

617

ABOUT THE AUTHOR Warren J. Smith, chief scientist at Kaiser ElectroOptics and an independent consultant, is one of the most widely known writers and educators in the field of optical design. He is the author of Modern Optical Engineering, Modern Lens Design, and Practical Optical System Layout.